THE MINOR PLANET

BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS

VOLUME 44, NUMBER 4, A.D. 2017 OCTOBER-DECEMBER 287.

PHOTOMETRIC OBSERVATIONS OF MAIN-BELT were operated at sensor temperature of –15°C and images were ASTEROIDS 1990 PILCHER AND 8443 SVECICA calibrated with dark and flat-field frames.

Stephen M. Brincat Both telescopes and cameras were controlled remotely from a Flarestar Observatory (MPC 171) nearby location via Sequence Generator Pro (Binary Star Fl.5/B, George Tayar Street Software). Photometric reduction, lightcurve construction, and San Gwann SGN 3160, MALTA period analyses were done using MPO Canopus software (Warner, [email protected] 2017). Differential aperture photometry was used and photometric measurements were based on the use of comparison stars of near- Winston Grech solar colour that were selected by the Comparison Star Selector Antares Observatory (CSS) utility available through MPO Canopus. Asteroid 76/3, Kent Street magnitudes were based on MPOSC3 catalog supplied with MPO Fgura FGR 1555, MALTA Canopus.

(Received: 2017 June 8) 1990 Pilcher is an inner main-belt asteroid that was discovered on 1956 March 9 by K. Reinmuth at Heidelberg. Also known as 1956 We report on photometric observations of two main-belt EE, this asteroid was named in honor of Frederick Pilcher, asteroids, 1990 Pilcher and 8443 Svecica, that were associate professor of physics at Illinois College, Jacksonville acquired from 2017 March to May. We found the (Illinois), who has promoted extensively, the interest in minor synodic rotation period of 1990 Pilcher as 2.842 ± planets among amateur astronomers (Schmadel & Schmadel, 0.001 h and amplitude of 0.08 ± 0.03 mag and of 8443 1992). The JPL (2017) Small-Bodies Database Browser lists the Svecica as 20.998 ± 0.001 h and amplitude of 0.62 ± diameter as 6.754 km ± 0.167 km based on H = 13.14. 0.03 mag

During 2017, photometric observations of two main-belt asteroids were carried out from two observatories located in Malta (Europe). The two asteroids for this research were selected through the CALL website (Warner, 2016).

Observations of 1990 Pilcher were obtained from Flarestar Observatory - MPC Code: 171 (14° 28m 12.4s E, 35° 54’ 37.2” N) through a 0.25-m f/6.3 Schmidt-Cassegrain (SCT) equipped with a Moravian G2-1600 CCD camera. Observations of 8443 Svecica were obtained through observations conducted from Antares Observatory (14° 30m 46.7s E, 35° 52’ 13.0” N) that used a 0.28- m SCT coupled to a SBIG ST-11000 CCD Camera. All images were taken through a clear filter and auto-guided for the duration of the exposure. Flarestar Observatory used the camera in 1x1 binning mode with a resultant pixel scale of 0.99 arcsec per pixel while Antares Observatory used its camera in 2x2 binning mode with a resultant pixel scale of 1.32 arcsec per pixel. Both cameras

Number Name yyyy /mm/ dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. Grp 1990 Pilcher 2017 03/18-04/13 134 4.7,2.5,10.6 185 -0.5 2.842 0.001 0.10 0.03 MB-I 8443 Svecica 2017 03/19-05/03 382 3.4,9.1,19.3 185 3.1 20.998 0.001 0.62 0.03 MB-M Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009). Minor Planet Bulletin 44 (2017) Available on line http://www.minorplanet.info/minorplanetbulletin.html 288

0.001h and amplitude of 0.62 ± 0.03 mag. The LCDB did not contain any references of the synodic period of this asteroid.

Acknowledgements

We would like to thank Brian Warner his work in the development of MPO Canopus and for his efforts in maintaining the CALL website. This research has made use of the JPL’s Small-Body Database.

References

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., Vilagi, J., Gajdos, S., Carbognani, A., Hornoch, K., Kusnirak, P., Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Observations conducted from Flarestar Observatory were carried Koehn, B.W. (2014). “On the maximum amplitude of harmonics out on four nights from 2017 March 18 to April 13. They of an asteroid lightcurve.” Icarus 235, 55-59. indicated a synodic period of 2.842 ± 0.001 h and amplitude of 0.08 ± 0.03 mag as the most likely solution based on a bimodal JPL (2017). Small-Body Database Browser - JPL Solar System lightcurve. However, if presuming that the asteroid has a non- Dynamics web site. http://ssd.jpl.nasa.gov/sbdb.cgi. bimodal lightcurve, the best solution would be 3.895 ± 0.001 h Last accessed: 2017 May 17. with amplitude of 0.10 ± 0.03. Schmadel, L.D., Schmadel, L.D. (1992). Dictionary of minor As discussed in Harris et al. (2014), the presumption of a bimodal planet names (p. 161). Berlin etc.: Springer. lightcurve does not always provide the correct solution since lightcurves with amplitudes of only 0.10 mag or so cannot be Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid assumed to be bimodal, even at low phase angles. Therefore, the Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Sep. 3.895 hour period cannot be overlooked and this leads us to http://www.minorplanet.info/lightcurvedatabase.html conclude that the results obtained for 1990 Pilcher are uncertain. There were no previous entries in the asteroid lightcurve database Warner, B.D. (2016). Collaborative Asteroid Lightcurve Link (LCDB, Warner et al., 2009) for this asteroid. website. http://www.minorplanet.info/call.html Last accessed: 2017 May 19. 8443 Svecica is a main-belt asteroid that was discovered by on 1977 October 16 by C.J. van Houten and I. van Houten- Warner, B.D. (2017). MPO Software, MPO Canopus v10.7.10.0. Groeneveld on Palomar Schmidt plates taken by T. Gehrel. This Bdw Publishing. asteroid was named for the small passerine bird - Luscinia svecica, http://www.minorplanetobserver.com/ also known as the Bluethroat. The JPL Small-Bodies Database Browser (JPL, 2017) lists the diameter of as 12.049 km ± 2.190 km when using H = 12.7. THE ROTATION PERIOD OF 10041 PARKINSON

John C. Ruthroff Shadowbox Observatory (H60) 12745 Crescent Drive Carmel, IN, USA 46032 [email protected]

(Received: 2017 April 29)

A rotation period of 5.69 h ± 0.03 h and an amplitude of 0.03 mag has been derived from one night of observations of main-belt asteroid 10041 Parkinson.

During the night of 2017 April 24 UT the author obtained 69 data points while observing main-belt asteroid 10041 Parkinson. Observations were made with a fork-mounted 0.30-m Schmidt- Cassegrain. The imaging train consisted of a SBIG AO-8T adaptive optics unit, a FW8G-STT filter wheel, and an SBIG STT- We observed 8443 Svecica on 11 nights between 2017 March 19 1603ME camera working at 2x2 binning, the resulting resolution and May 3. The data obtained for this asteroid were acquired on being 2.2 arc sec/pix. All observations were 300s. Camera sensor five nights at Antares Observatory and six nights at Flarestar temperature was –40°C. Due to the faintness of the target, no Observatory. Our analysis yielded a synodic period of 20.998 ± filters were used. All images were reduced with dark and flat

Minor Planet Bulletin 44 (2017) 289 frames. MPO Canopus v10.7.7.0 was used for differential Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid photometry and period analysis (see Ruthroff 2010, for technique Lightcurve Database.” Icarus 202, 134-146 Updated 2017 Apr 3. details). http://www.minorplanet.info/lightcurvedatabase.html

Data reduction reveals a probable rotation period of 5.69 h ± 0.03 h. A search of the Asteroid Lightcurve Database (LCDB; Warner et al., 2009) and the Astrophysics Data System did not find any previously reported results concerning the rotation period of 10041 Parkinson.

Acknowledgments

This paper makes use of data products from the Third U.S. Naval Observatory CCD Astrograph Catalog (UCAC3).

References

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Ruthroff, J.C. (2010). “Lightcurve Analysis of Main Belt Asteroids 185 Eunike, 567 Eleutheria, and 2500 Alascattalo.” Minor Planet Bul. 37, 158-159.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. Grp 10041 Parkinson 04/24 69 13.7 206 18 5.69 0.03 0.30 0.02 MBA Table I. Observing circumstances and results. Pts is the number of data points used in the analysis. The phase angle values are for the first and last date, unless a minimum (second value) was reached. LPAB and BPAB are the average phase angle bisector longitude and latitude. Period is in hours. Amp is peak-to-peak amplitude. LPAB and BPAB are the average phase angle bisector longitude and latitude (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009).

ASTEROID LIGHTCURVE ANALYSIS AT depending on the asteroid’s brightness and sky motion. Guiding CS3-PALMER DIVIDE STATION: on a field star sometimes resulted in a trailed image for the 2017 APRIL THRU JUNE asteroid.

Brian D. Warner Measurements were made using MPO Canopus. The Comp Star Center for Solar System Studies – Palmer Divide Station Selector utility in MPO Canopus found up to five comparison 446 Sycamore Ave. stars of near solar-color for differential photometry. Catalog Eaton, CO 80615 USA magnitudes were usually taken from the CMC-15 [email protected] (http://svo2.cab.inta-csic.es/vocats/cmc15/) or APASS (Henden et al., 2009) catalogs. The MPOSC3 catalog was used as a last resort. (Received: 2017 July 11) This catalog is based on the 2MASS catalog (http://www.ipac.caltech.edu/2mass) with magnitudes converted Lightcurves for 16 main-belt asteroids were obtained at from J-K to BVRI (Warner, 2007). The nightly zero points for the the Center for Solar System Studies-Palmer Divide catalogs are generally consistent to about ± 0.05 mag or better, but Station (CS3-PDS) from 2017 April thru June. Many of on occasion reach 0.1 mag and more. There is a systematic offset the asteroids were “strays” in the field of planned among the catalogs so, whenever possible, the same catalog is targets, demonstrating a good reason for data mining used throughout the observations for a given asteroid. Period images. Analysis shows that the Hungaria asteroid analysis is also done with MPO Canopus, which implements the (45878) 2000 WX29 may be binary. FALC algorithm developed by Harris (Harris et al., 1989).

In the plots below, the “Reduced Magnitude” is Johnson V as CCD photometric observations of 16 main-belt asteroids were indicated in the Y-axis title. These are values that have been made at the Center for Solar System Studies-Palmer Divide converted from sky magnitudes to unity distance by applying Station (CS3-PDS) from 2017 April thru June. Table I lists the –5*log (rΔ) to the measured sky magnitudes with r and Δ being, telescope/CCD camera combinations used for the observations. respectively, the Sun-asteroid and Earth-asteroid distances in AU. All the cameras use CCD chips from the KAF blue-enhanced The magnitudes were normalized to the given phase angle, e.g., family and so have essentially the same response. The pixel scales alpha(6.5°), using G = 0.15, unless otherwise stated. The X-axis is for the combinations range from 1.24-1.60 arcsec/pixel. the rotational phase ranging from –0.05 to 1.05. All lightcurve observations were unfiltered since a clear filter can result in a 0.1-0.3 magnitude loss. The exposure duration varied Minor Planet Bulletin 44 (2017) 290

Desig Telescope Camera Bernardus in 2017 is a mid-range value between the reported Squirt 0.30-m f/6.3 Schmidt-Cass ML-1001E extremes of 0.27-1.14 mag. The 0.20 mag amplitude for 6493 Borealis 0.35-m f/9.1 Schmidt-Cass FLI-1001E Cathybennett in 2017 fits within the reported range 0.19-0.23 mag. Eclipticalis 0.35-m f/9.1 Schmidt-Cass STL-1001E Australius 0.35-m f/9.1 Schmidt-Cass STL-1001E Zephyr 0.50-m f/8.1 R-C FLI-1001E Table I. List of CS3-PDS telescope/CCD camera combinations.

If the plot includes an amplitude, e.g., “Amp: 0.65”, this is the amplitude of the Fourier model curve and not necessarily the adopted amplitude for the lightcurve.

For the sake of brevity, only some of the previously reported results may be referenced in the discussions on specific asteroids. For a more complete listing, the reader is directed to the asteroid lightcurve database (LCDB; Warner et al., 2009). The on-line version at http://www.minorplanet.info/lightcurvedatabase.html allows direct queries that can be filtered a number of ways and the results saved to a text file. A set of text files of the main LCDB tables, including the references with bibcodes, is also available for download. Readers are strongly encouraged to obtain, when possible, the original references listed in the LCDB for their work.

596 Scheila. When observed in 2006 (Warner, 2006), this main- belt object was found to have a period of 15.848 h. There were no signs of unusual activity. On 2010 Dec 11, Steve Larson at the Catalina Sky Survey detected a “coma” around the asteroid, suggesting that it might be a cometary outburst. Follow-up observations eventually determined that the asteroid had been hit by a smaller object of about 35-m size (Jewitt et. al, 2011; Bodewits et al., 2011). When observed in 2011 (Warner, 2011a) and again in 2017, there were no signs of cometary activity. The 2017 observations led to a period of 15.793 h, but only by assuming previous results were correct.

1656 Suomi, 3022 Dobermann, 3266 Bernardus, 4490 Bambery, and 6493 Cathybennett. All of these Hungarias are “repeats” that were observed to provide additional data for spin axis modeling. The periods reported from the analysis of the most recent data are all in good agreement with previous results obtained by the author.

Observations in 2015 (Warner, 2016) suggested that 1656 Suomi might be binary, a secondary period of 12.6 hours with an amplitude of 0.11 mag being found. However, this was based on data from a single night that appeared to show an attenuation due to a satellite occultation/eclipse. Observations at previous apparitions as well as in 2017 found no similar “events.”

3022 Doberman and 4490 Bambery have always shown large amplitude lightcurves. The 0.49 mag amplitude for 3266

Minor Planet Bulletin 44 (2017) 291

of 20.18 h. There seems to be no reconciliation among the various results. A final solution awaits more data from future apparitions.

6674 Cezanne. There were no previously reported periods in the LCDB for this Nysa group member. The period of 3.37 h is reasonably secure, but additional observations are needed to confirm this result.

(16562) 1992 AV1. Finding a period for this Hungaria has been difficult. Previous results include Warner (2011b, 12.251 h or 6.51 h; 2014, 20.18 h). The data from 2017 led to entirely different result: 3.22 ± 0.01 h, which is close to the half-period of the alternate solution from 2011, when the amplitude was only 0.04 mag

Such divergent results prompted reviewing images from the (17014) 1999 CY96. This outer main-belt asteroid was a target of previous apparitions to be sure that the same asteroid had been opportunity in the field of a planned target. There were no worked each time. After confirming that this was the case, the reported periods in the LCDB. images from 2014 were measured anew. The revised data set led to a period of 34.85 h with a weak solution near the original period Minor Planet Bulletin 44 (2017) 292

(27000) 1998 BO44. This appears to be the first reported period (52586) 1997 PB. This Flora group member was a target of for this outer main-belt asteroid. The first night’s observations opportunity on two nights. The data set was sparse and noisy, were the result of the asteroid being in the same field as a planned leading to several possible solutions, two of which are shown target. The subsequent nights were follow-up after work on the below. The two periods differ by one rotation over a 24-hour planned target was finished. period. There were no other periods given in the LCDB.

(27097) 1998 UM26. Polishook et al. (2012) using data from four nights obtained by the Palomar Transient Factory reported a period of P > 8.7 h and amplitude of A > 0.07 mag. The CS3-PDS data from 2017 led to P = 6.651 h and A = 0.42 mag. This result is considered sufficiently secure to supplant the earlier result.

(56473) 2000 GY108. This is also a Flora group member that was a target of opportunity on two nights and had no previously- reported periods in the LCDB. Since each night covered most of the assumed lightcurve, and given the amplitude, the result is considered secure but not definitive. (51122) 2000 HN35. The error bars were very large for these observations (low SNR) and so are not shown in the lightcurve. Despite the larger errors, the result is considered reasonably secure because of the amplitude.

Minor Planet Bulletin 44 (2017) 293

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. Group 596 Scheila 06/01-06/13 922 0.9,6.6 249 0 15.793 0.005 0.06 0.01 MB-O 1656 Suomi 05/28-05/30 317 19.9,20.0 247 34 2.587 0.001 0.11 0.01 H 3022 Dobermann 06/20-06/26 211 19.1,19.8 261 33 10.329 0.001 0.77 0.02 H 3266 Bernardus 05/11-05/13 317 20.4,20.6 221 34 10.74 0.02 0.5 0.03 H 4490 Bambery 05/12-05/14 246 21.5,21.8 214 36 5.82 0.002 1.08 0.02 H 6493 Cathybennett 06/15-06/18 218 24.2,24.7 232 32 3.475 0.001 0.2 0.02 H 6674 Cezanne 05/11-05/14 75 23.6,23.8 160 4 3.37 0.01 0.3 0.03 NYSA 16562 1992 AV1 06/14-06/19 161 22.2,23.2 233 26 3.219 0.001 0.2 0.02 H 17014 1999 CY96 05/01-05/02 43 18.6,18.7 157 4 3.92 0.05 0.66 0.05 MB-O 27000 1998 BO44 05/05-05/16 217 5.4,4.7,4.8 232 13 11.034 0.003 0.34 0.03 MB-O 27097 1998 UM26 05/14-05/19 85 24.6,24.9 161 4 6.651 0.004 0.42 0.03 BAP 51122 2000 HN35 04/29-05/14 140 6.7,4.9 232 13 2.7378 0.0002 0.42 0.04 MB-O 52586 1997 PB 05/01-05/02 43 23.1,23.3 159 4 3.04 0.05 0.38 0.03 FLOR 56473 2000 GY108 04/16-04/16 73 4.6,4.6 210 6 7.01 0.05 0.52 0.03 FLOR 132450 2002 HT1 05/16-05/19 65 6.4,6.6 236 11 10.7 0.1 0.89 0.05 MB-I 247259 2001 RT98 05/03-05/05 68 11.2,10.8 241 20 6.69 0.01 0.75 0.05 MB-O

Table II. Observing circumstances and results. The phase angle (α) is given at the start and end of each date range. If three values are given, the middle one is the minimum phase angle during the range of observations. LPAB and BPAB are, respectively, the average phase angle bisector longitude and latitude (see Harris et al., 1984). The Group column gives the orbital group to which the asteroid belongs. The definitions and values are those used in the LCDB (Warner et al., 2009a). BAP = Baptistina; FLOR = Flora; H = Hungaria; MB-I/O = main- belt inner/outer.

6.69 h, is adopted here. Given the amplitude and low phase angle, this seems a reasonable assumption (Harris et al., 2014).

(132450) 2002 HT1. The period spectrum for this 1.4 km inner main-belt asteroid shows several secondary solutions and one primary. However, this is likely a “fit by exclusion,” which is where the Fourier analysis finds a minimum RMS by minimizing Acknowledgements the number of overlapping data points. Funding for observations, analysis, and publication for Warner and Stephens was provided by NASA grant NNX13AP56G. Work on the asteroid lightcurve database (LCDB) by Warner was also funded in part by National Science Foundation grant AST- 1507535. This research was made possible through the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund; and based in part on data from CMC15 Data Access Service at CAB (INTA-CSIC) (http://svo2.cab.inta-csic.es/vocats/cmc15/). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. (http://www.ipac.caltech.edu/2mass/)

References (247259) 2001 RT98. The estimated size of this outer main-belt Bodewits, D., Kelley, M.S., Li, J.-Y., Landsman, W.B., Besse, S., asteroid is 5.6 km. The period spectrum favored two solutions, a A’Hearn, M.F. (2011). “Collisional Excavation of Asteroid (596) monomodal and bimodal lightcurve. The latter, with a period of Scheila.” ApJ Letters 733, L3.

Minor Planet Bulletin 44 (2017) 294

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). ROTATION PERIOD DETERMINATIONS FOR “Lightcurves and phase relations of the asteroids 82 Alkmene and 46 HESTIA, 118 PEITHO, 333 BADENIA, 356 LIGURIA, 444 Gyptis.” Icarus 57, 251-258. AND 431 NEPHELE

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Frederick Pilcher Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, Organ Mesa Observatory (G50) H., Zeigler, K.W. (1989). “Photoelectric Observations of 4438 Organ Mesa Loop Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. Las Cruces, NM 88011 USA [email protected] Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., Vilagi, J., Gajdos, S., Carbognani, A., Hornoch, K., Kusnirak, P., (Received: 2017 June 13) Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B.W. (2014). “On the maximum amplitude of harmonics Synodic rotation periods and amplitudes are found for on an asteroid lightcurve.” Icarus 235, 55-59. 46 Hestia: 21.036 ± 0.001 h, 0.09 ± 0.01 mag; 118 Peitho: 7.805 ± 0.001 h, 0.14 ± 0.01 mag; 333 Badenia: Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, 9.862 ± 0.001 h, 0.24 ± 0.01 mag; 356 Liguria: 31.701 ± T.C., Welch, D.L. (2009). http://www.aavso.org/apass 0.001 h or 63.395 ± 0.002 h, 0.14 ± 0.01 mag; 431 Nephele: 13.530 ± 0.001 h, 0.13 ± 0.01 mag. Jewitt, D., Weaver, H., Mutcher, M., Larson, S., Agarwal, J. (2011). “Hubble Space Telescope Observations of Main Belt Comet (596) Scheila.” Ap. J. Letters 733, L4. Observations to obtain the data used in this paper were made at the Organ Mesa Observatory with a 0.35-meter Meade LX200 GPS Polishook, D., Ofek, E.O., Waszczak, A., Kulkarni, S.R., Gal- Schmidt-Cassegrain (SCT) and SBIG STL-1001E CCD. Yam, A., Aharonson, O., Laher, R., Surace., J., Klein, C., Bloom, Exposures were 60 seconds, unguided, with a clear filter. J., Brosch, N., Prialnik, D., Grillmair, C., Cenko, S.B., Kasliawal, Photometric measurement and lightcurve construction is with M., Law, N., Levitan, D., Nugent, P., Poznanski, D., Quimby, R.. MPO Canopus software. To reduce the number of points on the (2012). “Asteroid rotation periods from the Palomar Transient lightcurves and make them easier to read, data points have been Factory survey.” MNRAS 421, 2094-2108. binned in sets of 3 with a maximum time difference of 5 minutes.

Warner, B.D. (2006). “Asteroid lightcurve analysis at the Palmer 46 Hestia. Previously published rotation periods are by Scaltriti et Divide Observatory - late 2005 and early 2006.” Minor Planet al. (1981), 21.04 hours at celestial longitude 57 degrees; and by Bull. 33, 58-62. Pilcher (2012), 21.040 hours at celestial longitude 160 degrees. The lightcurves look almost identical with one deep minimum and Warner, B.D. (2007). “Initial Results of a Dedicated H-G one shallow minimum and amplitude 0.13 magnitudes. Program.” Minor Planet Bul. 34, 113-119.

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Updated 2017 April. http://www.minorplanet.info/lightcurvedatabase.html

Warner, B.D. (2011a). “Upon Further Review: VI. An Examination of Previous Lightcurve Analysis from the Palmer Divide Observatory.” Minor Planet Bull. 38, 96-101.

Warner, B.D. (2011b). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2010 December-2011 March.” Minor Planet Bull. 38, 142-149.

Warner, B.D. (2014). “Asteroid Lightcurve Analysis at CS3- Palmer Divide Station: 2014 January-March.” Minor Planet Bull. 41, 144-155.

Warner, B.D. (2016). “Asteroid Lightcurve Analysis at CS3- Palmer Divide Station: 2015 June-September.” Minor Planet Bull. 43, 57-65.

New observations were obtained on eight nights from 2017 May 2 to June 13 near celestial longitude 235 degrees. They provide a good fit to a lightcurve with an almost identical period 21.036 ± 0.001 h, but with smaller amplitude 0.09 ± 0.01 mag and two minima of nearly the same depth.

118 Peitho. The Asteroid Lightcurve Data Base (Warner et al., 2009) lists five independent published periods all between 7.78 hours and 7.823 hours, with the best value considered as 7.8055 hours.

Minor Planet Bulletin 44 (2017) 295

New observations on three nights from 2017 May 12-24 provide a good fit to a lightcurve with period 7.805 ± 0.001 h, amplitude 0.14 ± 0.01 mag. This is in excellent agreement with earlier results.

356 Liguria. The only previously published period is by Harris and Young (1980), 31.82 h with amplitude 0.22 mag. This is very close to 4/3 of the Earth’s rotation period. With this commensurability, observations should begin several weeks before opposition (2017 Mar. 20) and continue until several weeks afterward. The first new session was obtained on 2017 Feb 22.

Due to the need to observe other targets and bad weather, only five 333 Badenia. Previously published periods cluster around two sessions were obtained through April 3, and frequent observation different values. Those near 8.19 h are Blanco et al. (2000), did not begin until April 13. 8.160 h; Behrend (2005), 8.192 h; Behrend (2006), 8.19 h; and Behrend (2014), 8.2 h. Near to 9.86 hours are Denchev et al. To cover the entire lightcurve, individual sessions of at least eight (1999, republished 2000), 9.96 h; and Aznar et al. (2016), 9.860 h. hours in duration are needed. This is possible near opposition at It should be noted that six cycles of 8.2 hours each is 49.2 hours the declination of the target but not post opposition, i.e., April 13 – while five cycles of 9.86 hours each is a nearly identical 49.3 May 2. The total of 17 sessions 2017 Feb. 22 – May 3 are hours. Both are slightly more than two days. For a short interval of therefore poorly spaced in time. observation, an equally good fit can be made to both periods. This explains the ambiguity in the earlier observations.

New observations on six nights over the much longer interval of one month, 2017 Mar. 26 – Apr. 27, resolve the ambiguity. They provide an excellent fit to a lightcurve with a period of 9.862 ± 0.001 h, amplitude 0.24 ± 0.02 mag. The period spectrum is also provided, which shows that a period near 8.2 hours can be rejected.

Lightcurve of 356 Liguria phased to 31.701 hours and based on all sessions 2017 Feb. 22 - May 3.

Minor Planet Bulletin 44 (2017) 296

distinction between the two halves only in the maximum A. The discordance at A might favor an interpretation for the double period 63.395 hours, but the similarity of other parts of the lightcurve makes this interpretation less likely. The change in the maximum at A may be related to changes in phase angle.

Lightcurve of 356 Liguria phased to 63.395 hours and based on all sessions 2017 Feb. 22 - May 3.

The complete data set including all 17 sessions may be interpreted either in terms of a 31.701 hour period or a 63.395 hour period; results for each period are shown in accompanying figures.

When plotted to the longer period, the lightcurve has four maxima and minima. Alternate maxima denoted A, A’ have different Lightcurve of 356 Liguria phased to 31.686 hours and based on five appearances; alternate maxima denoted B, B’ are slightly sessions 2017 Feb. 22 - Apr. 3. different; all minima look the same within reasonable photometric error. A plot to 31.701 hours produces the usual bimodal lightcurve in which the two maxima A, A’ in the double period appear as a single maximum A and show significant discordance. All other corresponding segments of the double period lightcurve superpose well.

Lightcurve of 356 Liguria phased to 31.697 hours and based on eleven sessions 2017 Apr. 13 - May 3.

As shown in the accompanying figures, lightcurves plotted to near 31.7 hours separately for the five sessions 2017 Feb. 22 – Apr. 3 and for 11 sessions 2017 Apr. 13 – May 3 both lack full phase Split halves plot for 356 Liguria phased to 63.395 hours and based coverage but have no significant misfits. The lightcurve as shown on all sessions 2017 Feb. 22 - May 3. plotted to near 63.4 hours for 12 sessions 2017 Apr. 7 – May 3 has a large data gap, but available segments separated by one half A split halves plot (above) of the double period shows appreciable

Number Name 2017/mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp. A.E. 46 Hestia 05/02-06/13 1894 6.6,4.7,7.3 236 2 21.036 0.001 0.09 0.01 118 Peitho 05/12-05/24 800 6.8,11.5 216 1 7.805 0.001 0.14 0.01 333 Badenia 03/26-04/27 1713 2.1,0.9,7.9 192 -1 9.862 0.001 0.24 0.02 356 Liguria 02/22-05/03 5060 10.9,0.7,15.1 179 -1 31.701 0.001 0.14 0.01 431 Nephele 04/09-05/21 3854 12.1,0.8,1.9 236 2 13.530 0.001 0.13 0.01 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date, unless a minimum (second value) was reached. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

Minor Planet Bulletin 44 (2017) 297 cycle have no significant differences. A lightcurve plotted to near 63.4 hours for five sessions 2017 Feb. 22 – Apr. 3 is too fragmentary to provide information useful for resolving the period ambiguity. The maximum A in the 63.395 hour plot is defined by session 2544, March 21, 0.7 degrees phase angle; and session 2561, March 29, 4.0 degrees phase angle. The maximum A’ in the 63.395 hour plot is defined by sessions at larger phase angle: session 2570, April 7, 7.6 degree phase angle; and session 2608, May 1, 15.1 degrees phase angle. These data support a 31.70 hour period with the commonly encountered change of lightcurve shape with changing phase angle.

Acknowledgment

The author thanks Alan W. Harris for assistance in analyzing the data for 356 Liguria.

References

Aznar Macias, A., Carreno Garceran, A., Arce Mansego, E., Brines Rodriguez, P., Lozano de Haro, J., Fornas Silva, A., Fornas Silva, G., Mas Martinez, V., Rodrigo Chiner, O., Herrero Porta, D. (2016), “Twenty-one asteroid lightcurves at Group Observadores Lightcurve of 356 Liguria phased to 63.419 hours and based on de Asteroides (OBAS): Late 2015 to Early 2016.” Minor Planet twelve sessions 2017 Apr. 7 - May 3. Bull. 43, 257-263.

Summary and future work. I consider a period of 31.701 hours Behrend, R. (2002, 2005, 2006, 2014). Observatoire de Geneve with the usual bimodal lightcurve whose shape changes with web site. http://obswww.unige.ch/~behrend/page_cou.html. changing phase angle to be more likely, but cannot rule out the 63.395 hour period with four maxima and minima per cycle. Since Blanco, C., Di Martino, M., Riccioli, D. (2000). “New rotational the interval of observation is much longer than that published by periods of 18 asteroids.” Planet. Space Sci. 48, 271-284. Harris and Young (1980), the 31.701 hour period improves upon Denchev, P., Shkodrov, V., Ivanova, V. (1999). Abstracts of ACM the 31.82 hours in this source. With a period nearly 4/3 or 8/3 of 1999, 116-117. Earth period, single sessions of at least 8 hours are an absolute minimum for full phase coverage. As data near the start or end of Denchev, P., Shkodrov, V., Ivanova, V. (2000). “Synodic periods a session commonly have reduced photometric accuracy, single of asteroids 333, 402, 481, and 800.” Planet. Space Sci. 48, 983- sessions of 10 hours or longer are desired for good overlap. An 986. opportunity for such observations is presented near the 2021 Jan. 1 opposition near declination +37 degrees. Complete phase coverage Harris, A.W., Young, J.W. (1980). “Asteroid rotation. III – 1978 of the double period near 63.4 hours should be achieved in a short observations.” Icarus 43, 20-32 time interval in which there is very small change in the phase angle. Observations at widely separated longitude, that is a global Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). collaboration, are strongly encouraged. “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258. 431 Nephele. Previously published periods are by Behrend (2002), 21.43 h; and Wang et al. (2010), 18.821 h. New observations on Pilcher, F. (2012). “Rotation Period Determinations for 46 Hestia, 20 nights from 2017 Apr. 9 – May 21 provide a good fit to a 223 Rosa, 225 Henrietta, 266 Aline, 750 Oskar, and 765 lightcurve with period 13.530 ± 0.001 h, amplitude 0.13 ± 0.01 Mattiaca.” Minor Planet Bull. 39, 171-173. mag, and rule out both previously published periods. Scaltriti, F., Zappala, V., Harris, A.W. (1981). “Photoelectric Lightcurves and Rotation Periods of the Asteroids 46 Hestia and 115 Thyra.” Icarus 46, 275-280.

Wang, X.-b., Gu, S.-h., and Li, X.-j. (2010). “The Rotational Periods of Three C-type Asteroids 431, 521, and 524.” Earth, Moon, and Planets 106, 97-104.

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Updated 2017 Jan. 23. http://www.MinorPlanet.info/lightcurvedatabase.html.

Minor Planet Bulletin 44 (2017) 298 ROTATION PERIOD FOR (332660) 2008 WL7 Acknowledgements

J.A.G. Davalos This work was possible thanks to CONIDA, the Institute of Comisión Nacional de Investigación y Desarrollo Aeroespacial- Astronomy of the UNAM, and Universidad Autónoma de Nuevo CONIDA León (UANL). This work was based upon observations carried out Lima, PERU at the Observatorio Astronómico Nacional on the Sierra San Pedro [email protected] Mártir (OAN-SPM), Baja California, México.

J.S. Silva References Instituto de Astronomía-UNAM Ensenada, Mexico, km 103, Carr. Tijuana Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). Ensenada, B.C., MEXICO “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258. F.J. Tamayo Facultad de Ciencias Físico Matemáticas UANL Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Pedro de Alba, Ciudad Universitaria, 66451 San Nicolás de los Poutanen, M., Scaltriti, F., Zappalà, V., Schober, H.J., Debehogne, Garza, N.L., MEXICO H., Zeigler, K.W. (1989). “Photoelectric Observation of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. J.W. Schuster Instituto de Astronomía-UNAM Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Ensenada, Mexico, km 103, Carr. Tijuana Lightcurve Database.” Icarus 202, 134-146. Updated 2017 April. Ensenada, B.C., MEXICO http://www.minorplanet.info/lightcurvedatabase.html

F.I. Alvarez Universidad Autónoma de Baja California Carretera Tijuana- Ensenada 3917, Playitas, 22860 Ensenada, B.C., MEXICO

(Received: 2017 May 8)

The asteroid (332660) 2008 WL7 was observed on 2017 March 8. The synodic period was found to be 2.54 ± 0.15 h.

The outer main-belt asteroid (332660) 2008 WL7 was observed on 2017 March 8 for about 2.5 hours with the 2.12-m f/7.5 Ritchey- Chretien telescope of the National Astronomical Observatory in San Pedro Mártir-Mexico (OAN-SPM). The CCD camera was a Spectral with 2048x2048x13.5 micron pixels that was binned 2x2. This configuration gave a field-of-view of approximately 6x6 arcmin and an image scale of 0.176 arcsec/pix. An R filter was used; the exposure time was 90 s.

The calibration images were reduced using IRAF (Image Reduction and Analysis Facility). For photometry we used MaxIm DL (Diffraction Limited). The raw plot of the data shows the magnitude versus light-time corrected UT. The relative magnitude was obtained by subtracting the instrumental magnitude of the asteroid from that of a comparison star in the same field that was about the same brightness as the asteroid.

The phased lightcurve shows that full coverage was obtained on the single night. The peak-to-peak amplitude is about 0.10 mag. The period was found fitting a Fourier series to the data following the methodology of Harris et al. (1989). The best solution was obtained with fourth-order fit with a period of 2.54 ± 0.15 h. A search of the asteroid lightcurve database (Warner et al., 2009) did not find a previously reported result. The observational circumstances and results are summarized in Table I.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. Grp 332660 2008 WL7 08/03 69 8.75,8.67 195 4 2.54 0.15 0.10 0.01 MB

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009).

Minor Planet Bulletin 44 (2017) 299

LIGHTCURVE ANALYSIS FOR al., 2009) and Pan-STARRS (Magnier et al., 2016) catalogues (for 341 CALIFORNIA, 594 MIREILLE, 1115 SABAUDA, faint stars only) to set the zero-points each night. This process 1504 LAPPEENRANTA, AND 1926 DEMIDDELAER took into consideration the number of nights of measurement and the internal scatter reported in the catalogues. We also checked for Tom Polakis obvious variables in the TASS MkIV survey (Droege et. al., 2006) Command Module Observatory and in VSX (Watson et al., 2006). For V-band photometry the 121 W. Alameda Dr. ASAS-3 (Pojmanski 2002) catalogue was also queried. These data Tempe, AZ 85282 USA were found using the CDS VizieR catalogue-query service [email protected] (VizieR, 2017), the ASAS-3 query page, and the Pan-STARRS search page at the Space Telescope MAST archive. In most Brian A. Skiff regions the Sloan r´ data sources for brighter stars yielded very Lowell Observatory similar magnitudes (within about 0.05 mag total range), so we Flagstaff, AZ USA took mean values rounded to 0.01 mag precision. We usually adopted only the higher-accuracy Pan-STARRS or SDSS DR7 (Received: 2017 May 11) data for stars fainter than about r´ = 13.5 and 15.0, respectively.

Synodic rotation periods were determined for five main- This careful adjustment of the comp star magnitudes and color- belt asteroids: 341 California, 317 h with suspected indices allowed the separate nightly runs to be linked often with tumbling; 594 Mireille, 4.9671 ± 0.0004 h; 1115 no zero-point offset required, or shifts of only a few hundredths of Sabauda, 6.7165 ± 0.0007 h; 1504 Lappeenranta, a magnitude in a series. 15.16 ± 0.01 h; and 1926 Demiddelaer, 32.095 ± 0.027 h. All the data have submitted to the ALCDEF Nearly always we used 9-pixel (16 arcsec) diameter measuring database. apertures for the V02 data. The apertures used on the 0.7-m data varied depending on seeing, but were typically 13 or 15 pixels (12 or 14 arcsec) diameter. When necessary we made use of the MPO CCD photometric observations of five main-belt asteroids were Canopus ‘Star-B-Gone’ feature to subtract the effects of performed at Command Module Observatory (MPC V02) in contaminating field stars, usually successfully. For most of the Tempe and the Lowell Observatory Anderson Mesa Station (MPC asteroids described here, we note the RMS scatter on the phased 688) outside Flagstaff. Images at V02 were taken using a 0.32-m lightcurves, which gives an indication of the overall data quality f/6.7 Modified Dall-Kirkham telescope, SBIG STXL-6303 CCD including errors from the calibration of the frames, measurement camera, and either a Cousins R or ‘clear’ glass filters. Exposure of the comp stars, the asteroid itself, and the actual period-fit. times for all the images were 3 minutes. The image scale after 2x2 binning was 1.76 arcsec/pixel. Images taken at 688 employed the The uncertainties on the period-determination are from the MPO 0.7-m f/8 telescope, which has a CCD camera system designed Canopus Fourier-type FALC fitting method (cf. Harris et al., and built in the Lowell instrument shop (Buie, 2010). The image 1989). It is worth noting that recently Dykhius et al. (2016, their scale was 0.91 arcsec/pixel with 2x2 binning. Either Johnson V or Appendix B) have checked the reliability of the error estimates Cousins R filters were used for the asteroid observations. Table I resulting from the FALC method, and find from Monte Carlo tests shows the observing circumstances and results. that they are realistic one-sigma errors.

The V02 images were calibrated using a dozen bias, dark, and flat The Asteroid Lightcurve Database (LCDB; Warner et al., 2009) frames. Flat-field images were made using an electroluminescent was consulted to locate previously published results. Finally, we panel. The 688 data made use of 20 full-frame biases and 15 or note that all our new data are deposited in the ALCDEF database. more twilight flats taken each night under an automated exposure routine with the telescope aimed at the ‘Chromey spot’ (Chromey 341 California. This Flora-family asteroid was discovered in 1892 et al., 1996), tracked at the sidereal rate but dithered 30" between by Max Wolf at Heidelberg. Due to its slow rotation, the correct frames. The thinned, back-illuminated e2v CCD was kept at period was poorly determined until recently. Behrend (2005) first roughly –110° C using a Cryotiger chiller and so had negligible reported a period of 8.74 ± 0.05 h. This, however, was based on dark current. only two isolated nights in 2005; a single follow-up night in 2008 January yielded the same erroneous period (Behrend, 2008). Skiff The data reduction and period analysis were done using MPO (2014) reported a preliminary result, to be described below, Canopus (Warner, 2017). The asteroid and three to five showing the period to be nearly two weeks long. More recently comparison stars were measured, preserving comp stars among Pilcher et al. (2017) acquired an excellent, uniform six-month adjacent nights if possible (more readily done with the 45'x30' series in the second half of 2016. This allowed them to confirm field of the V02 CCD). We attempted to keep the comparison star that the principal rotation period near 317 h reported by Skiff was colors within the range roughly 0.5 < B-V < 0.95, or equivalent correct, and to identify a secondary “tumbling” period of some “asteroidal” color-ranges in other photometric systems, though 250 h. this was not always possible. In order to reduce the internal scatter in the data, we typically chose the brightest stars of appropriate The asteroid was followed from 2013 December through 2014 color that had peak ADU counts below the range where chip March at Lowell using the LONEOS 0.55-m f/1.9 Schmidt camera response becomes nonlinear in both cameras. (MPC 699) for the first two nights only (unfiltered), and then the 0.7-m telescope (Rc filter) in robotic mode for the remaining 28 Although the MPO Canopus internal star catalogue helped in nights. Since the period was clearly going to be long, data were selecting comp stars, we adopted magnitudes from a combination obtained on several discrete visits each night rather than making of CMC15 (Muiñoz et al. 2014), APASS DR9 (Munari et al. continuous runs, similar to what Pilcher et al. have done. The 2015), GAIA1 G magnitudes (Sloan r´ = G + 0.066 for stars of resulting lightcurve showing a period of 317 hours was posted to asteroidal color), as well as the original SDSS DR7 (Abazajian et the CALL site (Skiff 2014). At the time the data were reduced

Minor Planet Bulletin 44 (2017) 300 approximately to the Sloan r´ system, which has now been revised for both telescopes using more recent photometric catalogues. The first phased plot shows the data from the 2014 apparition with an order-6 fit. The correction to the magnitudes of the comp stars reduces the observed brightness range to 0.58 mag. (originally 0.75 mag.).

Three additional isolated nights in 2016 were obtained at V02 and at 688 to seek short-period variations (cf. Warner, 2016). Like Pilcher et al., we found none. These are included in the ALCDEF files.

594 Mireille. This asteroid was discovered in 1906, also by Max Wolf at Heidelberg. The orbit has moderately high inclination and Another series using the 0.7-m telescope and V filter was obtained eccentricity. The only previous period determination was by the following year, 2015 Feb-Apr. The data were adjusted as Wisniewski (1991), who found a period of 4.966 h and an closely as possible to standard Johnson V magnitudes. The amplitude of 0.18 mag from observations in early 1988. lightcurve for this apparition shows much stronger effects from tumbling. The second phased plot is a force-fit to the 317-hour We obtained 352 data points from both V02 and 688 on five period, where the tumbling effects are obvious. The brightness nights in 2017 April with the asteroid at +50° ecliptic latitude, range is about 0.54 mag. well north in the morning sky. All data were reduced to Sloan r´. These yielded a rotation period of 4.9671 ± 0.0004 h, in excellent agreement with Wisniewski’s period. The lightcurve morphology is similar to that of Wisniewski. The full amplitude is 0.25 ± 0.01 mag; the RMS scatter on the order-4 fit shown in the phased plot is 0.012 mag.

Taking advantage of anomalously clear summer weather in the Southwest US, a third run of 656 data points was acquired at V02 on fourteen consecutive nights beginning on 2016 July 3. The data thus cover just one cycle. Again we show a force-fit to the 317 h period. The data, taken mainly in groups of three 3-minute exposures, are binned here into 10-minute means. The magnitude 1115 Sabauda. This outer main-belt asteroid was discovered in scale is Sloan r´ and the full amplitude is 0.92 mag. at this higher 1928 by Luigi Volta at Pino Torinese. Four similar rotational phase angle. periods have been published. Warner (2006) obtained a period of 6.72 ± 0.01 h. Behrend (2005) and Behrend (2015) show results of 6.75 ± 0.01 h and 6.66 ± 0.02 h, respectively. Finally, Ruthroff (2013) shows a period of 6.72 ± 0.01 h.

Sufficient data to produce a lightcurve for 1115 Sabauda was secured on three nights at V02 in 2017 March. From 146 data-

Minor Planet Bulletin 44 (2017) 301 points we find a period of 6.7165 ± 0.0007 h, in close agreement with the previous results. The phased plot shows an order-6 fit, which has a full amplitude of 0.22 ± 0.01 mag, and RMS scatter of 0.011 mag.

1926 Demiddelaer. This Eunomia-family asteroid was discovered by Eugène Delporte at Uccle in 1935. Only one period determination has been published, that of Behrend (2008), who computed 18.5 ± 0.3 h. 1504 Lappeenranta. This is an inner main-belt asteroid, discovered During eight nights in 2017 March, 525 images of 1926 by Liisi Oterma at Turku in 1939. The LCDB shows four disparate Demiddelaer were acquired at V02. An unambiguous period of rotational periods with the highest ‘U’ value only 2+. Binzel 32.095 ± 0.027 h was computed from these, which differs (1987) published a period of 10.44 ± 0.10 h and amplitude 0.29 substantially from the previously published one. The phased plot mag from just sixteen measurements on three consecutive nights at shows an order-5 fit to the data binned into 10-minute averages. McDonald Observatory. Results from Behrend (2002, 2006) are The amplitude is again small, only 0.08 ± 0.01 mag, and the RMS given approximately as 8 h. Most recently Garlitz (2013) derived a scatter on the fit is 0.010 mag. period of 15.190 ± 0.009 h and amplitude 0.22 mag.

A total of 637 images from ten nights at V02 in 2017 March were used to determine the period of rotation of 1504 Lappeenranta. Both single and double-mode fits produced acceptable solutions. We therefore show two phased lightcurves, one for 15.16 ± 0.01 h and 30.34 ± 0.02 h. Both plots have the groups of 3 x 3-minute exposures averaged into 10-minute bins. While the single-mode period agrees with Garlitz, the lightcurve morphology differs significantly. The amplitude during 2017 March was only 0.09 ± 0.01 mag, and the RMS scatter on both fits is 0.009 mag.

Acknowledgments

The authors would like to express our gratitude to Brian Warner for his advice on use of MPO Canopus and in the analysis and interpretation of the lightcurves.

References

Abazajian, K.N., Adelman-McCarthy, J.K., Agueros, M.A., Allan, Sahar, S., Allende Prieto, C., An, D., Anderson, K.S.J., Anderson,

S.F., Annis, J., Bahcall, N.A., and 194 coauthors (2009). “The seventh data release of the Sloan Digital Sky Survey.” Astrophys. J., Suppl. Ser. 182, 543-558.

Minor Planet Bulletin 44 (2017) 302

Number Name 20yy/mm/dd Pts Phase LPAB BPAB Period (h) P.E. Amp A.E. Obs 341 California 13/12/12-14/03/31 1284 8.3,24.4,22.0 77 5 317.0 0.2 0.58 0.03 BS 341 California 15/02/11–15/04/23 375 21.8,2.1,17.4 173 4 317.0 0.1 0.54 0.03 BS 341 California 16/07/03-16/07/17 656 34.9,34.1 355 -5 317.0 0.1 0.92 0.03 TP 594 Mirelle 17/04/03-17/04/11 352 33.8,33.7 165 20 4.9671 0.0004 0.25 0.01 TP,BS 1115 Sabauda 17/03/09-17/03/15 146 8.9,9.5 235 42 6.7163 0.0007 0.22 0.01 TP 1504 Lappeenranta 17/03/09-17/03/24 637 10.9,9.9,10.5 177 16 15.16 0.01 0.09 0.01 TP 1504 Lappeenranta 17/03/09-17/03/24 637 10.9,9.9,10.5 177 16 30.34 0.02 0.09 0.01 TP 1926 Demiddelaer 17/03/09-17/03/22 525 9.5,9.4,10.4 172 18 32.095 0.027 0.08 0.01 TP Table I. Observing circumstances and results. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum or maximum, which is then the second of three values. LPAB and BPAB are each the average phase angle bisector longitude and latitude (see Harris et al., 1984). The Obs. column gives the observer.

Behrend, R. (2002, 2005, 2006, 2008, 2015). Observatoire de Muiñoz, J.L., Evans, D.W. (2014). “The CMC15, the last issue of Geneve web site. the series Carlsberg Meridian Catalogue, La Palma.” Astron. http://obswww.unige.ch/~behrend/page_cou.html Nach. 335, 367.

Binzel, R.P. (1987). “A photoelectric survey of 130 asteroids.” Ochsenbein, F., Bauer, P., Marcout, J. (2000). “The VizieR Icarus 72, 135-208. database of astronomical catalogues.” Astron. Astrophys., Suppl. Ser. 143, 23-32. Buie, M.W. (2010). “Converting from Classical to Robotic Astronomy: The Lowell Observatory 0.8-m Telescope.” Adv. in Pilcher, F., Franco, L., Pravec, P. (2017). “319 Leona and 341 Astron. California – Two Very Slowly Rotating Asteroids.” Minor Planet https://www.hindawi.com/journals/aa/2010/130172 Bull. 44, 87-90.

Chromey, F.R., Hasselbacher, D.A. (1996). “The Flat Sky: Pojmanski, G. (2002). “The All Sky Automated Survey. Catalog Calibration and Background Uniformity in Wide Field of Variable Stars. I. 0h - 6h Quarter of the Southern Hemisphere.” Astronomical Images.” PASP 108, 944-949. Acta Astron. 52, 397-427.

Droege, T.F., Richmond, M.W., Sallman, M.P., Creager, R.P. Ruthroff, J.C. (2013). “Lightcurve Analysis of Main Belt (2006). “TASS Mark IV Photometric Survey of the Northern Asteroids 1115 Sabauda 1554 Yugoslavia, 1616 Filipoff, 2890 Sky.” PASP 118, 1666-1678. Vilyujsk, (5153) 1940 GO, and (31179) 1997 YR2.” Minor Planet Bul. 40, 90-91. Dykhuis, M.J., Molnar, L.A., Gates, C.J., Gonzales, J.A., Huffman, J.J., Maat, A.R., Maat, S.L., Marks, M.I., Massey- Skiff, B.A. (2014). Posting on CALL site. Plantinga, A.R., and 8 coauthors. (2016). “Efficient spin-sense http://www.minorplanet.info.call.html determination of Flora-region asteroids via the epoch method.” Icarus 267, 174-203. VizieR (2017). http://vizier.u-strasbg.fr/viz-bin/VizieR Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and Warner, B.D. (2006). “Asteroid lightcurve analysis at the Palmer 444 Gyptis.” Icarus 57, 251-258. Divide Observatory - March - June 2006.” Minor Planet Bul. 33, 85-88. Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid H., Zeigler, K.W. (1989). “Photoelectric Observations of Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Feb. Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. http://www.minorplanet.info/lightcurvedatabase.html

Garlitz, J. (2013). Elgin Observatory web site. Warner, B.D. (2016). "Three Additional Candidates for the Group http://users.eoni.com/~garlitzj/Period.htm of Very Wide Binaries.” Minor Planet Bul. 43, 306-309.

JPL (2017). Small-Body Database Browser. Warner. B.D. (2017). MPO Canopus software. http://ssd.jpl.nasa.gov/sbdb.cgi#top http://bdwpublishing.com

Magnier, E.A., Schlafly, E.F., Finkbeiner, D.P., Tonry, J.L., Watson C., Henden, A.A., Price, A. (2006). “The AAVSO Goldman, B., Roser, S., Schilbach, E., Chambers, K.C., International Variable Star Index.” The Society for Astronomical Flewelling, H.A., Huner, M.E., and 11 coauthors. (2016). “Pan- Sciences 25th Annual Symposium on Telescope Science 25, 47. STARRS Photometric and Astrometric Calibration.” https://arxiv.org/abs/1612.05242. Ap. J., submitted. Wisniewski, W.Z. (1991). “Physical studies of small asteroids. I - Lightcurves and taxonomy of 10 asteroids.” Icarus 90, 117-122. Munari, U., Henden, A., Frigo, A., Zwitter, T., Bienayme, O., Bland-Hawthorn, J., Boeche, C., Freeman, K.C., Gibson, B.K., Gilmore, G., Grebel, E.K., Helmi, A., Kordopatis, G., Levina, S.E., and 13 coauthors. (2015). “APASS Landolt-Sloan BVgri photometry of RAVE stars. I. Data, effective temperatures, and reddenings.” Astron. J., 148, 81.

Minor Planet Bulletin 44 (2017) 303 ROTATION PERIOD DETERMINATION FOR 213 LILAEA References

Frederick Pilcher Di Martino, M., Dotto, E., Celino, A., Barucci, M.A., Fulchignoni, Organ Mesa Observatory (G50) M. (1995). “Intermediate size asteroids: Photoelectric phtometry 4438 Organ Mesa Loop of 8 objects.” Astron. Astrophys. Suppl. Ser. 112, 1-7. Las Cruces, NM 88011 USA [email protected] Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and Lorenzo Franco 444 Gyptis.” Icarus 57, 251-258. Balzaretto Observatory (A81) Rome, ITALY Zeigler, K.W. (1987). “Photoelectric photometry of asteroids 213 Lilaea and 376 Geometria.” Minor Planet Bull. 14, 11-12. Caroline Odden, Sydney Marler, Lydia Paris, Noah S. Ward, Victor Yung Phillips Academy Observatory 180 Main Street Andover, MA 01810 USA

(Received: 2017 May 18)

CCD photometry of 213 Lilaea in April-May 2017 yields a synodic rotation period 12.042 ± 0.001 hours and a lightcurve amplitude of 0.20 ± 0.02 magnitudes.

Two previously published rotation periods of 213 Lilaea are both based on sparse lightcurves covering only a short time interval. These periods are by Zeigler (1987), 7.85 hours; and by Di Martino et al. (1995), 8.045 hours. A. W. Harris and B. D. Warner examined the lightcurve by Di Martino et al. (1995), considered their 8.045 hour period to be unreliable, and recommended a more comprehensive study. Observations from a wide range of geographical longitudes (Franco in Europe, Phillips Academy Observatory in eastern North America, and Pilcher in western North America) were necessary to achieve full phase coverage for a period very nearly Earth commensurate.

Pilcher at Organ Mesa Observatory used a 35 cm Meade LX200 GPS, SBIG STL-1001E CCD, clear filter. Franco at Balzaretto Observatory used a 20 cm Meade LX200 SCT, SBIG ST7XME CCD. The Phillips Academy Observatory used a 40 cm DFM Engineering f/8 R-C, Andor Tech iKon DW 436C CCD, clear filter.

Observations on eleven nights 2017 Apr. 5 – May 11 provide a good fit to an irregular lightcurve with period 12.042 ± 0.001 hours, amplitude 0.20 ± 0.02 magnitudes. A period spectrum is also provided, and a period near 8.045 hours is definitively ruled out.

Acknowledgments

Research at the Phillips Academy Observatory is supported by the Israel Family Foundation. Many thanks to the Abbot Academy Association for the generous grant used to purchase the new Andor Tech camera.

Number Name 2017/mm/dd Pts Phase LPAB BPAB Period(h) P.E Amp A.E. 213 Lilaea 04/05-05/11 1342 14.8, 20.4 156 +5 12.042 0.001 0.20 0.02 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first date and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

Minor Planet Bulletin 44 (2017) 304

LIGHTCURVE OBSERVATIONS OF NINE MAIN-BELT ASTEROIDS

Johan Warell Lindby Observatory (K60) Lindby 229, SE-274 93 Skurup, SWEDEN [email protected]

(Received: 2017 May 23)

Photometric observations of nine main-belt asteroids were obtained in 2014-2016. The selected objects all had

unusually favourable apparitions. Lightcurves and 2042 Sitarski. A period of 2.63 h and an amplitude of 0.36 mag rotation periods are presented for 1911 Schubart, 2042 were found for this object from three nights of observations. One Sitarski, 2383 Bradley, 3000 Leonardo, 4974 Elford, session covers the full period and indicates a bimodal and highly 5471 Tunguska, 8679 Tingstäde, (16206) 2000 CL39 asymmetric light curve. A competing period of 2.78 h was found and (24691) 1990 RH3. with nearly as low RMS. More observations are needed.

The observations of nine main-belt asteroids were carried out at Lindby Observatory (MPC code K60) in southernmost Sweden. Images were obtained with a 0.25-m f/10 Schmidt-Cassegrain (SCT) operating at f/4.6, a Starlight Xpress SXV-H9 CCD camera, and a clear imaging filter. The pixel scale was 2.3 arc seconds and image exposure times were 45, 120 or 180 seconds. All images were calibrated with bias, flats and darks. Lightcurve analysis and photometric reduction to the V filter band were made with MPO Canopus software using the MPOSC3 star catalog and the Photometry Magnitude Method (Warner 2014). With the Canopus Comparison Star Selector, up to five comparison stars with near- solar colors were used to derive differential magnitudes for each image. Within Canopus, the FALC routine (Harris et. al., 1989) 2383 Bradley. This object clearly has an asymmetric bimodal was used to fit multi-night observations and compute synodic lightcurve that is well-determined with good overlap between the rotation periods for the targets. two sessions. The period is 5.83 h with 0.67 mag. amplitude.

The observations and targets are summarized in Table I. Using the CALL web site, targets were selected primarily near favourable oppositions and had neither notified nor submitted previous observations. Unless otherwise noted, a search of the asteroid lightcurve database (LCDB; Warner et al. 2009) and the web identified no previously reported lightcurves of these objects.

1911 Schubart. This is a well-observed target with a single-peak light curve of small amplitude, 0.11 mag. The reported period of 7.91 h is covered fully in one of the observing sessions and has a pronounced RMS minimum. Black et al. (2016) and Hess et al. (2016) observed this target but did not report a period. Stephens (2016) reported a period of 11.915 h based on a longer time series; 3000 Leonardo. The period determination is uncertain since full this period cannot be verified with the present data. phase coverage is lacking and the number of data points is small. The most likely period is 8.54 h with an amplitude of 0.55 mag. Periods of 7.21 h and 10.40 h are other possibilities. Hayes- Gehrke et al. (2016) reported a period of 7.52 h and amplitude of 0.28 mag with a data set with better phase coverage and less noise.

Number Name yyyy mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 1911 Schubart 2015 02/26-03/10 143 7.4, 11.0 134,5 -1,1 7.91 0.02 0.11 0.03 2042 Sitarski 2015 12/01-12/09 37 18.0, 21.3 29,3 +2,4 2.63 0.01 0.36 0.05 2383 Bradley 2014 03/12-04/11 95 7.8, 10.5 184,0 +0,9 5.823 0.003 0.67 0.05 3000 Leonardo 2015 12/01-12/09 38 22.1, 24.7 31,9 -1,4 8.54 0.05 0.55 0.05 4974 Elford 2015 04/09-04/16 248 5.5, 5.2 204,1 +8,8 6.56 0.02 0.41 0.05 5471 Tunguska 2015 08/24-09/02 154 18.9, 18.8 56,3 +3,9 5.17 0.01 0.25 0.05 8679 Tingstäde 2016 09/07-09/12 143 9.8, 7.3 5,4 +0,0 6.65 0.03 0.63 0.07 16206 2000 CL39 2016 09/07-09/12 148 9.5, 7.5 6,1 -1,2 7.21 0.04 0.28 0.10 24691 1990 RH3 2016 09/07-09/12 130 10.0, 7.5 5,8 -1,7 6.76 0.05 0.30 0.10

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

Minor Planet Bulletin 44 (2017) 305

mag) was found at a clear RMS minimum in the period search. Four sessions covered the full period with ample overlap.

4974 Elford. The period with the marginally lowest RMS for this object, 3.28 h, is considered unlikely since it represents a unimodal light curve. The most likely period of 6.56 h produces a nice bimodal, slightly asymmetric, lightcurve that has an RMS (24691) 1990 RH3. A period of 9.33 h and amplitude of 0.50 mag only 1 % larger. The amplitude is 0.41 mag. were found for this object. The scatter is significant but the RMS minimum is quite pronounced, with session overlap across almost the full period. Half-period and double-period solutions in the period spectrum have significantly larger RMS values.

5471 Tunguska. A well-fit period of 5.17 h gives an undulating lightcurve with one minimum and one maximum. The amplitude is 0.25 mag. Two sessions marginally covered the full period. References

Black, S., Linville, D., Michalik, D., Wolf, M., Ditteon, R. (2016). “Lightcurve analysis of asteroids observed at the Oakley Southern Sky Observatory” Minor Planet Bulletin 43, 287-289. CALL (2017). Collaborative Asteroid Lightcurve Link web site, http://www.minorplanet.info/call/ Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Hess, K., Bruner, M., Ditteon, R. (2016). “Asteroid lightcurve 8679 Tingstäde. The scatter is significant in the photometry and analysis at the Oakley Southern Sky Observatory: 2015 February- the period spectrum shows a single pronounced RMS minimum. March.” Minor Planet Bulletin 44, 3-5. The lightcurve, P = 6.65 h, has single maximum with a large Hayes-Gehrke, M.N., Ceballos, B., Kinds, S., Choic, J., Sison, P., amplitude of 0.63 mag. Marbukh, M., Wu, J., Sciamanna, J., Riley, T., Cydulkin, Y., Mullen R., Gallagher, D., Ravin, N., Nudel-Linetsky, M., Alston, Al-L., Ortel, A. (2016). “Photometric analysis of 3000 Leonardo.” Minor Planet Bulletin 43, 119. JPL Small Body Database Browser (2017). http://ssd.jpl.nasa.gov/sbdb.cgi Stephens, R.D. (2016). “Asteroids observed from CS3: 2016 April - June.” Minor Planet Bulletin 43, 336-338. Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database". Icarus 202, 134-146. Updated 2017 April. http://www.MinorPlanet.info/lightcurvedatabase.html (16206) 2000 CL39). A period of 7.21 h with a shallow minimum Warner, B.D. (2016). MPO Software, MPO Canopus version and maximum in an otherwise flat lightcurve (amplitude 0.29 10.7.7.0. Bdw Publishing, http://minorplanetobserver.com/

Minor Planet Bulletin 44 (2017) 306 LIGHTCURVE ANALYSIS FOR 2142 LANDAU

Melissa N. Hayes-Gehrke, Kade Arrington, Josh Brady, Sabrina Christian, Symon Ginsburg, Destiny McLeod-Campbell, Christian Musial, Andrew Pham, Duncan Woodward Department of Astronomy University of Maryland College Park, MD 20742 [email protected]

(Received: 2017 June 8)

Lightcurve analysis using MPO Canopus of three nights of observations of 2142 Landau produced a tentative rotation period of 19.2 ± 0.2 h, supporting a previous determination of 19.4 h.

Asteroid 2142 Landau was discovered on 1972 April 3 by L. I. Chernykh at the Crimean Astrophysical Observatory and named in memory of Lev Davydovich Landau. It is a main-belt asteroid with an orbital period of 5.64 years, absolute magnitude of 12.0, geometric albedo of 0.05, and a diameter of 20.1 km (MPC 5284).

Observations were conducted remotely from telescopes operated by iTelescope.net. The telescope used on 2017 April 3 and 6 was T17 (MPC Q62), located at the Siding Spring Observatory. The coordinates of T17 are 31° 16’ 24” S and 149° 03’ 52” E. T17 has an array of 1024 pixels by 1024 pixels, a primary diameter of 0.43 m, a focal length of 2917 mm, pixel size of 13 microns by 13 microns, and a full well of 100,000 e-. There were 13 usable images from 2017 April 3 and 12 usable images from 2017 April 6. The telescope used on 2017 April 5 was T11 (MPC H06), located at the New Mexico Skies Observatory. The coordinates of T11 are 32° 54’ 13” N and 105° 31’ 42” W. T11 has an array of 4008 pixels by 2672 pixels, a primary diameter of 0.5 m, a focal length of 2280 mm, pixel size of 9 microns by 9 microns, and a full well of 60,000 e-. There were 58 usable images from 2017 Acknowledgements April 5. Images taken had an exposure of 300 seconds each, using a clear/luminance filter with binning set to 1. We used periodic Telescope time and research was funded by the Department of recentering to keep our telescope pointed at 2142 Landau. The Astronomy, University of Maryland, College Park. Observations data were analyzed through MPO Canopus using the lightcurve were conducted by the ASTR315 class of Spring 2017, taught by wizard to perform aperture and differential photometry. Dr. Melissa Hayes-Gehrke at the University of Maryland, College Park. The two facilities used were operated remotely through the Previously published work by Chang et al (2016) found a possible iTelescope service. rotation period of 9.7 ± 0.2 h. The Lightcurve Database (LCDB) also lists a second possible period of 19.4 h. Neither reference References provided lightcurves, due to being part of a mass analysis of many asteroids from a survey program. Chang, Chan-Kao et al. “Large Super-Fast Rotator Hunting Using The Intermediate Palomar Transient Factory.” The Astrophysical The largest amount of data we obtained was on 2017 April 5 over Journal Supplement Series 227.2 (2016): 20. a period of 4 hours. These data show a steady upward trend for the entire observing period, with possible peaking near the end, so we NASA JPL. “JPL Small-Body Database Browser.” Solar System believe that the second period determined by Chang et al (2016) Dynamics. NASA JPL, 23 Oct. 2007. of 19.4 h is more likely. The fitted curves in MPO Canopus https://ssd.jpl.nasa.gov/sbdb.cgi support this, as we found a fit for 19.2 ± 0.2 h. However, due to Warner, B.D. “Asteroid Lightcurve Database (LCDB).” limited observing time, phasing to such a long period leaves large MinorPlanet.info. MinorPlanet.info, 4 Apr. 2017. Web. 08 May gaps in the plot, so our fit is not definitive. However, our data do 2017. http://www.minorplanet.info/PHP/lcdbsummaryquery.php provide a first look at parts of this asteroid’s lightcurve.

Number Name 2017 mm/dd Pts Phase Period(h) P.E. Amp 2142 Landau 04/03-04/06 83 3.5 19.2 0.2 0.2 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for range between first and last date.

Minor Planet Bulletin 44 (2017) 307

Warner, B.D. MPO Software, MPO Canopus version 10.7.7.0 iTelescope.net. “Remote Internet Telescope Network - Online Bdw Publishing, 22 Jul. 2016 Imaging & Telescope Hosting Service.” Telescope 11. http://minorplanetobserver.com iTelescope.net, n.d. Web. 08 May 2017. http://www.itelescope.net/telescope-t11/ iTelescope.net. “Remote Internet Telescope Network - Online Imaging & Telescope Hosting Service.” Telescope 17. iTelescope.net, n.d. Web. 08 May 2017. http://www.itelescope.net/telescope-t17/

THE ROTATION PERIOD OF 1117 REGINITA Waszczak, A., Chang, C.-K., Ofek, E.O., Laher, R., Masci, F., Levitan, D., Surace, J., Cheng, Y.-C., Ip, W.-H., Kinoshita, D., Hanjie Tan Helou, G., Prince, T.A., Kulkarni, S. (2015). “Asteroid Light Department of Optoelectric Physics Curves from the Palomar Transient Factory Survey: Rotation Chinese Culture University Periods and Phase Functions from Sparse Photometry.” Astron. J. No.55 Hwa-Kang Rd., Taipei, TAIWAN 150, A75. [email protected]

Bin Li Purple Mountain Observatory No.2 Beijing West Rd., Nanjing, CHINA PR

Xing Gao Xinjiang Astronomical Observatory 150 Science 1-Street Urumqi, Xinjiang, CHINA PR

(Received: 2017 May 15)

The lightcurve of main-belt asteroid 1117 Reginita was determined using images taken at Xingming Observatory (C42) on four nights in 2017 Jan. Analysis of the observations shows a bimodal solution with a synodic rotation period of 2.946 ± 0.001 h and an amplitude of 0.15 mag.

The main-belt asteroid 1117 Reginita was discovered by Josep Comas Solá on 1927 May 29 at Barcelona, Spain. It was named in honor of the niece of its observer. The most recent work by Waszczak et al. (2015) found a rotation period P = 2.9275 ± 0.0134 h with and amplitude of 0.10 mag in R band

The four nights of observations we report were all made at Xingming Observation (C42) using 0.5-m f/4 reflector telescope with an unfiltered QHY11 CCD at 2x2 binning. Exposures were 90 sec. The image scale of was 1.8 arcsec/pixel. All images were calibrated with flat, dark, and bias frames using Maxim DL.

MPO Canopus was used to analyze the data. Based on a data set of 477 data points, we found a period of 2.946 ± 0.001 h with an amplitude of 0.15 mag. This agrees with the period found by Waszczak et al. (2015).

References

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. D 1117 Reginita 01/02-01/07 477 6.9,4.7 117 -3 2.946 0.001 0.15 0.02 5.1

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). D is the estimated diameter (km).

Minor Planet Bulletin 44 (2017) 308

LIGHTCURVE AND ROTATION PERIOD FOR MINOR PLANET 2504 GAVIOLA

Dr. Melissa Hayes-Gehrke, David Linko, Raghav Bhasin, James Johnson, Brian Bermudez, Iryna Fedorenko, Katie Tillis, Nicole Villar Department of Astronomy University of Maryland College Park , MD [email protected]

(Received: 2017 June 8 )

CCD photometric observations using iTelescope T21 of asteroid 2504 Gaviola were made in April 2017. A Acknowledgements rotation period of 8.751 ± 0.003 h and lightcurve Funding for observations were provided by the Astronomy amplitude of 0.31 mag was determined from two nights Department at the University of Maryland. We would also like to of observations. thank iTelescope for their facilities to study the asteroid.

The main-belt asteroid 2504 Gaviola was discovered in 1967 by References Carlos Ulrrico Cesco and Arnold R. Klemola at Astronomical Bus, S.J., Binzel, R.P. (2002). “Phase II of the Small Main-Belt facility Leoncito in Argentina and named in honor of Asteroid Spectroscopic Survey.” Icarus 158, 106–145. astrophysicist Ramón Enrique Gaviola. Its orbital period is 4.59 years. The absolute magnitude H = 12.0 and assumed albedo of Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., 0.301 give a diameter of 10.579 km (JPL, 2017). 2504 Gaviola has Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, been assigned a taxonomic classification of Sq-type by Bus and H., Zeigler, K.W. (1989). “Photoelectric Observations of Binzel (2002) during Phase II of the small main-belt asteroid Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. spectroscopic survey of 2002. iTelescope (2017) iTelescope.Net - Remote Internet Telescope The observations were made using iTelescope T21 located in Network - Online Image & Telescope Hosting Services. Mayhill, New Mexico (MPC code H06) on 04/04 and 04/19. http://www.itelescope.net/ Observations were made with a Planewave 0.43-m Corrected Dall Kirkham (CDK) telescope operating at f/4.5 using a FLI-PL6303E JPL (2017). Small-Body Database Browser - JPL Solar System CCD camera with a 3072 x 2048 array of 9-micron pixels. The Dynamics web site. http://ssd.jpl.nasa.gov/sbdb.cgi resulting images were 0.96 arcsec per pixel. All images were mid- exposure times light-time corrected using MPO Canopus 10.7.7.0. Warner, B.D. (2016). MPO Software, MPO Canopus version A total of 85 data points were used in the calculation. Table I 10.7.7.0, Bdw Publishing. http://www.minorplanetobserver.com/ includes observing conditions and the determined results. Data analysis was conducted in MPO Canopus using differential Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid photometry. Accurate results were achieved by selecting five Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Sep. comparison stars using the “comp star selector” feature of the http://www.minorplanet.info/lightcurvedatabase.html lightcurve wizard. The period analysis was completed using MPO Canopus’s lightcurve analysis that incorporates the Fourier Waszczak, A., et al. (2015). Asteroid Light Curves from the analysis algorithm developed by Harris (Harris et al. 1989). Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry. Astron. J. 150, 75. The phased lightcurve demonstrates a classical tri-axial shape by the asteroid. The period determination of 8.751 ± 0.003 h is in close agreement with the value present in the Small Body Database. The rotation period for this asteroid was initially determined by Waszczak et al. (2015) as a part of a survey for large number of asteroids. The period of 8.751 h determined here is not uniquely distinct, because there were many different alternatives due to aliases between our ~8-h observing window and the asteroid’s ~8-h rotation period. This period however, complies with the earlier observations and provides a first look at this asteroid’s lightcurve.

Number Name 2017 mm/dd Pts Phase Period(h) P.E. Amp Grp

2504 Gaviola 04/04-04/19 085 3.6 8.751 0.003 0.31 MB-O Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the mid date. Grp is the asteroid family/group (Warner et al., 2009).

Minor Planet Bulletin 44 (2017) 309 LIGHTCURVE FOR ASTEROID 4404 ENIRAC

Dr. Melissa N. Hayes-Gehrke, Rosemary Caffes, Anthony Gibson, Alex Honer, Ryan Hunter, Tracey Paul, Coleman Quimby, Thomas Riffe, Mark Roberts, Jack Schemmel, Uchechukwu Unaegbu, Zachary Wilton Department of Astronomy, University of Maryland College Park, Maryland 20742 [email protected]

(Received: 2017 June 8)

CCD observations made of the asteroid 4404 Enirac during 2017 April led to a lightcurve with a rotation period of 2.9979 ± 0.0003 h and an amplitude of 0.27 mag.

Asteroid 4404 Enirac is a main-belt object that was discovered by A. Maury at Palomar on 1987 April 2 (JPL, 2013). The T21 telescope at the Mayhill, New Mexico observatory (MPC H06) was used for the asteroid lightcurve research we report for this asteroid. The telescope is located at 32° 54’ N and 105° 31’ W and is at an elevation of 2,225 meters above sea level. The telescope is a Planewave CDK that has a diameter 0.43 meters. The CCD is a FLI-PL6303E and the CCD are 3072 by 2048 pixels, which are 9�m square in size. iTelescope software was used to control the telescope on observing nights. Each image was taken with 300-s exposure through a luminance filter. A total of 105 usable images were taken on the nights of 2017 March 30, April 2, 5 and 17. MPO Canopus version 10.7.7.0 was used to analyze our data.

The fitted lightcurve of 4404 Enirac yields a rotation period of 2.9979 ±0.0003 h, which refines a previous determination by Klinglesmith III, Jesse Hanowell, Janek Turk, Angelica Vargas and Curtis Alan Warren, who found a rotation period of 2.998 ±0.002 h. The scattered points from 2017 April 5 were likely caused by the bright sky due to a waning gibbous moon.

Acknowledgements

This research was made possible by data collected using the iTelescope network and funding by the University of Maryland, College Park.

References

Klinglesmith III, D.A., Hanowell, J., Turk, J., Vargas, A., and Warren, C.A. (2014). “Asteroid Observations at Etscorn: Mid- 2013.” Minor Planet Bulletin 41, 15-16. iTelescope - T21 - Mayhill, New Mexico http://www.itelescope.net/telescope-t21/

JPL (2013). Small-body database browser. https://ssd.jpl.nasa.gov/sbdb.cgi#top

Warner, B.D. (2013). MPO Software, MPO Canopus version 10.7.7.0, Bdw Publishing. http://www.minorplanetobserver.com /MPOSoftware/MPOCanopus.htm

Number Name 2017 mm/dd Pts Phase Period(h) P.E. Amp 4404 Enirac 03/30-04/17 105 21.8 2.9979 0.0003 0.27 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the mid-date. Period is the rotation period in hours. P.E. is the period error and Amp is amplitude.

Minor Planet Bulletin 44 (2017) 310

LIGHTCURVE ANALYSIS FOR NEAR-EARTH ASTEROID (138404) 2000 HA24

Melissa N. Hayes-Gehrke, Jack de La Beaujardiere, Prathamesh Kotgire, Austin Piel, Miles King, Kenneth Tran, Jackson Kenyon, David Hagen, Liam Fulling, Jason Walters, Alexander Acuna Department of Astronomy University of Maryland College Park, MD 20742 USA [email protected]

(Received: 2017 June 8)

Lightcurve analysis of asteroid (138404) 2000 HA24 from a single night of observation, 2017 April 17, yielded an estimated rotation period of 3.8 ± 0.2 h, with an amplitude of 0.3 mag. Figure 2. Observations of (138404) 2000 HA24 phased to a period of 3.7768 h

Asteroid (138404) 2000 HA24 was originally discovered on 2000 One point of data from an image taken at 17:56 UTC on April 17 April 28 at LINEAR- Lincoln Laboratory ETS in New Mexico. It was excluded due to its unusually high brightness, attributed to a has an eccentricity of 0.319 and a semi-major axis of 1.140 AU hot pixel. As can be seen from the raw plot (Fig. 1), the data (JPL, 2016). No previous rotation period was found in the exhibit significant scatter, created by the faintness of the asteroid Lightcurve Database (Warner, B.D. 2015). and consequent low-signal-to noise ratio for the measurements. Some of the early images in the session were not centered and the The T17 telescope (MPC Q62) located in Siding Spring, Australia asteroid moved through the field of view quickly. This limited the (iTelescope, 2017) was used for the observations on 2017 April number of comparison stars available, creating some uncertainty 17. It is a 0.43-m f/6.8 reflector + CCD. It is equipped with a FLI in the aperture photometry results. The results presented in Figure ProLine E2V CCD47-10-1-109 CCD, which has a pixel array of 2 used four comparison stars and an order of 2 in the Fourier 1024×1024 pixels of size 13×13 microns. The telescope was model used to fit a sinusoidal curve to the points by MPO accessed through itelescope.net, and exposures of 300s were taken Canopus (Warner, 2013); the fitted period is 3.8 ± 0.2 h. through the luminance filter. Acknowledgements

This research was funded by the Astronomy department at the University of Maryland, College Park. The observations were conducted using internet telescopes provided by iTelescope at the Siding Spring Observatory in New South Wales, Australia. We would like to thank Dr. Tony Farnham of the University of Maryland for his help in determining asteroid 138404 2000 HA24’s rotation period.

References

iTelescope (2017). http://www.itelescope.net/telescope-t17/

JPL (2006). Small-Body Database Browser https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=138404 Figure 1. Raw data from 2017 March 17 Warner, B.D. (2013). MPO Software, MPO Canopus version 10.7.7.0. Bdw Publishing. http://bdwpublishing.com/

Warner, B.D. (2015). “The Asteroid Lightcurve Database.” http://www.minorplanet.info/lightcurvedatabase.html

Number Name 2017 mm/dd Pts Phase Period(h) P.E. Amp. (138404) 2000HA24 04/27 54 24.1 3.7768 0.2319 0.30 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the date.

Minor Planet Bulletin 44 (2017) 311

ROTATION PERIODS FOR THREE MAIN BELT ASTEROIDS

Lorenzo Franco Balzaretto Observatory (A81), Rome, ITALY [email protected]

Giorgio Baj M57 Observatory (K38), Saltrio, ITALY

Vito Tinella N.A.R.O Observatory (K65), Cesena, ITALY

Mauro Bachini, Giacomo Succi Santa Maria a Monte (A29), ITALY

Giovanni Battista Casalnuovo Eurac Observatory (C62), Bolzano, ITALY Paolo Bacci 1602 Indiana is a S-type inner main-belt asteroid, discovered on San Marcello Pistoiese (104), Pistoia, ITALY 1950 March 14 at the Goethe Link Observatory at Brooklyn, IN. Collaborative observations of this asteroid were made over four (Received: 2017 July 3) nights. There are three previously published rotation periods determinations, ranging from 2.570 to 2.610 h with amplitudes Photometric observations of three main-belt asteroids ranging from 0.12 to 0.19 mag. More details are reported into were made from Italy in order to determine their synodic lightcurve database (LCDB; Warner et al., 2009). We derive a rotation periods. For 1022 Olympiada the period is synodic period of P = 2.601 ± 0.001 h with an amplitude A = 0.16 3.834 ± 0.001 hr, amplitude 0.66 mag. For 1602 Indiana ± 0.05 mag, consistent with the previously published results. the results are 2.601 ± 0.001 hr and 0.16 mag. and for 2501 Lohja we report 3.809 ± 0.001 hr and 0.44 mag.

A collaborative observing campaign was organized by the asteroids section of the UAI (Italian Amateur Astronomers Union) in order to involve its members into asteroid photometry projects. For this purpose we selected some asteroids with known and fast rotation periods. The CCD observations for three main-belt asteroids were made in March-April 2017 using the instrumentation described in Table I. Lightcurve analysis were made at the Balzaretto Observatory with MPO Canopus (BDW Publishing, 2016). All the images were calibrated with dark and flat frames and converted to R magnitudes using solar colored field stars from CMC15 catalogue, distributed with MPO Canopus. Table II shows the observing circumstances and results.

1022 Olympiada is a X-type middle main-belt asteroid discovered on 1924 June 23 by Albitzkij, V. at Simeiz Observatory. Collaborative observations of this asteroid were made over three nights. There are six previously published rotation periods 2501 Lohja is an A-type inner main-belt asteroid discovered on determinations, ranging from 3.822 to 3.835 h with amplitudes 1942 April 14 by Oterma, L. at Turku. Collaborative observations ranging from 0.27 to 0.46 mag. More details are reported into of this asteroid were made over two nights. There are twelve lightcurve database (LCDB; Warner et al., 2009). We derive a previously published rotation periods determinations, ranging synodic period of P = 3.834 ± 0.001 h with an amplitude A = 0.66 from 3.804 to 3.810 h with amplitudes ranging from 0.26 to 0.45 ± 0.05 mag. This period is consistent with the previous ones and mag. More details are reported into lightcurve database (LCDB; the high amplitude is explained by the observed equatorial aspect, Warner et al., 2009). We derive a synodic period of P = 3.809 ± evaluated as an angle of 96°, using the spin axis solution by Hanus 0.001 h with an amplitude A = 0.44 ± 0.05 mag, consistent with et al. (2011; Lambda = 46°, Beta = 10°). the previously published results.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E Amp A.E. 1022 Olympiada 03/14-03/16 942 14.7,15.3 140 15 3.834 0.001 0.66 0.05 1602 Indiana 03/17-03/28 402 17.0,21.4 150 6 2.601 0.001 0.16 0.05 2501 Lohja 03/30-04/03 153 21.0,22.1 145 2 3.809 0.001 0.44 0.05 Table II. Observing circumstances and results. Pts is the number of data points. The phase angle values are for the first and last date.

LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

Minor Planet Bulletin 44 (2017) 312

LIGHTCURVE ANALYSIS OF L4 TROJAN ASTERIODS AT THE CENTER FOR SOLAR SYSTEM STUDIES 2017 APRIL - JUNE

Robert D. Stephens Center for Solar System Studies (CS3)/MoreData! 11355 Mount Johnson Ct., Rancho Cucamonga, CA 91737 USA [email protected]

Brian D. Warner Center for Solar System Studies (CS3) MoreData! Eaton, CO

(Received: 2017 July 7)

Lightcurves for eight Jovian Trojan asteroids were obtained at the Center for Solar System Studies (CS3) from 2017 April to June. References CCD Photometric observations of eight Trojan asteroids from the Hanuš, J., Ďurech, J., Brož, M., Warner, B. D., Pilcher, F., L4 (Trojan) Lagrange point were obtained at the Center for Solar Stephens, R., Oey, J.; Bernasconi, L., Casulli, S., Behrend, R., System Studies (CS3, MPC U81). For several years, CS3 has been Polishook, D., Henych, T., Lehký, M., Yoshida, F., Ito, T. (2011). conducting a study of Jovian Trojan asteroids. This is another in a “A study of asteroid pole-latitude distribution based on an series of papers reporting data being accumulated for family pole extended set of shape models derived by the lightcurve inversion and shape model studies. It is anticipated that for most Jovian method”, Astronomy & Astrophysics 530, A134. Trojans, two to five dense lightcurves per target at oppositions well distributed in ecliptic longitudes will be needed and can be Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). supplemented with reliable sparse data for the brighter Trojan “Lightcurves and phase relations of the asteroids 82 Alkmene and asteroids. For most of these targets, we were able to get 444 Gyptis.” Icarus 57, 251-258. preliminary pole positions and create shape models from sparse data and the dense lightcurves obtained to date. These preliminary Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid models will be improved as more data are acquired at future lightcurve database.” Icarus 202, 134-146. Updated 2017 April. oppositions and will be published at a later date. http://www.minorplanet.info/lightcurvedatabase.html Table 1 lists the telescopes and CCD cameras that were used to Warner, B.D. (2016). MPO Software, MPO Canopus v10.7.7.0. make the observations. Images were unbinned with no filter and Bdw Publishing. http://minorplanetobserver.com had master flats and darks applied. The exposures depended upon various factors including magnitude of the target, sky motion, and Observatory Moon illumination. (MPC code) Telescope, CCD Observed Asteroids K38 0.30-m RCT f/5.8, 1022, 1602, 2501 Telescope Camera SBIG ST10ME 0.40-m F/10 Schmidt-Cass FLI Proline 1001E 0.35-m F/11 Schmidt-Cass Fli Microline 1001E K65 0.40-m SCT f/5.6, 1022, 1602, 2501 0.35-m F/10 Schmidt-Cass SBIG STL-1001E SBIG ST9XE Table 1. List of telescopes and CCD cameras used at CS3. A29 0.40-m NRT f/5, 1022, 2501 DTA EL-260E Image processing, measurement, and period analysis were done C62 0.30-m f/4 NRT, 1022, 1602 using MPO Canopus (Bdw Publishing), which incorporates the QHY9 Fourier analysis algorithm (FALC) developed by Harris (Harris et 104 0.60-m f/4 NRT, 1022 al., 1989). Night-to-night calibration (generally < ±0.05 mag) was Apogee Alta done using field stars from the CMC-15 catalog or APASS (Henden et al., 2009) The Comp Star Selector feature in MPO Table I. Observing Instrumentations. SCT: Schmidt-Cassegrain. Canopus was used to limit the comparison stars to near solar RCT: Ritchey-Chretien, NRT: Newtonian Reflector. color.

In the lightcurve plots, the “Reduced Magnitude” is Johnson V corrected to a unity distance by applying -5*log (r∆) to the measured sky magnitudes with r and ∆ being, respectively, the Sun-asteroid and the Earth-asteroid distances in AU. The magnitudes were normalized to the phase angle given in parentheses using G = 0.15. The X-axis rotational phase ranges from -0.05 to 1.05.

The amplitude indicated in the plots (e.g. Amp. 0.23) is the amplitude of the Fourier model curve and not necessarily the adopted amplitude of the lightcurve. Minor Planet Bulletin 44 (2017) 313

Targets were selected for this L4 observing campaign based upon the availability of dense lightcurves acquired in previous years. We obtained 2 to 4 lightcurves for most of these Trojans at previous oppositions, and some data were found from the Palomar Transient Factory, Waszczak et al., (2015).

For brevity, only some of the previously reported rotational periods may be referenced. A complete list is available at the lightcurve database (LCDB; Warner et al., 2009).

To evaluate the quality of the data obtained to determine how much more data might be needed, preliminary pole and shape models were created for all of these targets which will be published at a later date. Sparse data observations were obtained from the Catalina Sky Survey and USNO-Flagstaff survey using the AstDyS-3 site (http://hamilton.dm.unipi.it/asdys2/). This sparse data was combined with our dense data as well as any other dense data found in the Asteroid Lightcurve Database 4060 Deipylos. Using sparse photometry from the Palomar (http://www.alcdef.org/) using MPO LCInvert, (Bdw Publishing) a Transient Factory, Waszczak et al. (2015) reported a period of Windows-based program that incorporates the algorithms 11.4905 h for Deipylos. That period appears to be a 5:4 alias of the developed by Kassalainen et al (2001a, 2001b) and converted by period of rotation period of 9.3 h periods we found in 2015 and Josef Durech from the original FORTRAN to C. A period search 2016 (Stephens et al., 2015 and 2016b). This year’s finding of was made over a sufficiently wide range to assure finding a global 9.38 h is in good agreement. minimum in χ2 values.

2920 Automedon. This large Trojan has been studied in the past. Molnar et al. (2008) and Mottola et al., (2011) each found synodic rotational periods near 10.2 h. The result found this year is in good agreement.

4068 Menestheus. We studied this asteroid on three previous occasions: French et al. (2013) and Stephens et al. (2016a and 2016b), each time finding a period near 14.4 h. The result this year of 14.40 h is in good agreement with those findings.

3709 Polypoites. We observed this Trojan three times in the past (French et al. 2011, Stephens et al. 2016a, Stephens et al. 2016b). The 2016 observations enabled us to resolve aliases and determine the period over all three oppositions to be about 10.04 h. The period found this year of 9.989 h supports that conclusion.

4833 Meges. The synodic period we found this year agrees with previous synodic results (Mottola et al., 2011, Stephens et al., 2016b).

Minor Planet Bulletin 44 (2017) 314

2016b) finding rotation periods near 41 h with a bimodal shape to the lightcurves. However, with amplitudes of only 0.10 and 0.16 mag. respectively, it is possible that the lightcurve could have only a single extrema, or three or more extrema (Harris et al 2014). During a preliminary shape model attempt using the 2015 and 2016 data, we identified an alias in the period of about 21 h. The data obtained this year again found aliases at 21 h and 41 h with the 21 h period having a slightly stronger solution in the Period Spectrum. The 2017 21 h solution also produced the classic bimodal shape while phasing it to 41 h resulted in four extrema. Rephasing the 2015 and 2016 data to 21 h results in monomodal lightcurves. For these reasons, we now adopt the 21.43 h solution as more likely. However, additional observations in the future are needed to help resolve the ambiguities.

(11395) 1998 XN77. Mottola et al. (2011) observed this Trojan in 2009 and 2010, finding periods of 13.70 h and 13.696 h, respectively. We first observed the asteroid in 2015 using the 0.9- m SMARTS telescope at CTIO and then in a follow-up session using the 0.35-m telescope at CS3 (Stephens et al., 2016b), finding a period of 17.89 h. We observed it again in 2016 from CS3, obtaining a much denser data set, and found a period of 17.383 h with a classic bimodal shaper to the lightcurve. Determining a rotation period with the 2015 data proved difficult because of the low amplitude and strong aliases. We were able to rephase the 2015 data to this period, but because of the low amplitude, many rotation periods were possible. The rotational period found this year was 17.44 h period, consistent with the shorter period found in 2016.

(15440) 1998 WX4. We observed this Trojan in 2013 (French et al., 2013) and 2014 (Stephens et al., 2014). In both cases, the raw lightcurves spanning multiple nights were featureless. We observed it again in 2015 and 2016 (Stephens et al., 2016a and

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 2920 Automedon 06/04-06/14 364 3.3,2.8 263 13 10.223 0.003 0.11 0.02 3709 Polypoites 06/20-06/23 191 5.1,5.5 251 20 9.989 0.007 0.18 0.02 4060 Deipylos 06/30-07/05 204 3.6,4.1 269 17 9.38 0.02 0.11 0.02 4068 Menestheus 07/02-07/04 159 5.7,5.9 259 19 14.49 0.01 0.26 0.02 4833 Meges 06/25-06/30 286 6.0,6.6 249 21 12.285 0.004 0.44 0.02 11395 1998 XN77 05/20-05/30 384 4.9,4.0 254 18 17.44 0.01 0.11 0.02 15440 1998 WX4 06/01-06/18 482 4.8,4.4,4.5 260 22 21.43 0.02 0.09 0.02 15527 1999 YY2 05/01-05/05 144 6.2,5.7 243 22 6.987 0.003 0.39 0.02 Table II. Observing circumstances and results. Pts is the number of data points. Phase is the solar phase angle for the first and last date. If there are three values, the middle value is the minimum phase angle. LPAB and BPAB are, respectively, the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

Minor Planet Bulletin 44 (2017) 315 References

French, L.M., Stephens, R.D., Lederer, S.M., Coley, D.R., Rohl, D.A. (2011). “Preliminary Results from a Study of Trojan Asteroids.” Minor Planet Bul. 38, 116-120.

French, L.M., Stephens, R.D., Coley, R., Wasserman, L.H., Vilas, F., La Rocca, D. (2013). “A Troop of Trojans: Photometry of 24 Jovian Trojan Asteroids.” Minor Planet Bul. 40, 198-203.

Galad, A., Kornos, L., Vilagi, J.,\ (2010). “An Ensemble of Lightcurves from Modra.” Minor Planet Bul. 37, 9-15.

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.

Harris, A.W., Pravec, P., Galád, B. Skiff, B., Warner, B., Világi, J., Gajdoš, S., Carbognani, A., Hornoch, K., Kušnirák, P., Cooney, W., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B. (2014). “On the maximum amplitude of harmonics of an asteroid lightcurve.” Icarus 235, 55-59.

Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, T.C., Welch, D.I. (2009). http//www.aavso.org/apass

Kassalainen, M., Torppa J. (2001a). “Optimization Methods for Asteroid Lightcurve Inversion. I. Shape Determination.” Icarus 153, 24-36.

(15527) 1999 YY2. Galad et al. (2010) previously observed this Kassalainen, M., Torppa J., Muinonen, K. (2001b). “Optimization Trojan finding a rotational period of 6.9903 h. Our finding agrees Methods for Asteroid Lightcurve Inversion. II. The Complete with that result. Inverse Problem.” Icarus 153, 37-51.

Molnar, L.A., Haegert, M.J., Hoogeboom, K.M. (2014). “Lightcurve Analysis of an Unbiased Sample of Trojan Asteroids.” Minor Planet Bul. 35, 82-84.

Mottola, S., Di Martino, M., Erikson, A., Gonano-Beurer, M., Carbognani, A., Carsenty, U., Hahn, G., Schober, H., Lahulla, F., Delbò, M., Lagerkvist, C. (2011). “Rotational Properties of Jupiter Trojans. I. Light Curves of 80 Objects.” Astron. J. 141, A170.

Stephens, R.D., French, L.M., Davitt, C., Coley, D.R. (2014). “At the Scaean Gates: Observations Jovian Trojan Asteroids, July- December 2013.” Minor Planet Bul. 41, 95-100.

Stephens, R.D., Coley, D.R., French, L.M. (2015). “Dispatches from the Trojan Camp - Jovian Trojan L5 Asteroids Observed from CS3: 2014 October - 2015 January.” Minor Planet Bul. 42,

216-224. Acknowledgements Stephens, R.D., Coley, D.R., French, L.M. (2016a). “Large L5 Work on the asteroid lightcurve database (LCDB) was also funded Jovian Trojan Asteroid Lightcurves from the Center for Solar in part by National Science Foundation grants AST-1210099 and System Studies.” Minor Planet Bul. 43, 15-22. AST-1507535. This research was made possible in part based on data from CMC15 Data Access Service at CAB (INTA-CSIC) Stephens, R.D., Coley, D.R., Warner, B.D., French, L.M., (http://svo2.cab.inta-csic.es/vocats/cmc15/) and through the use of (2016b). “Lightcurves of Jovian Trojan Asteroids from the Center the AAVSO Photometric All-Sky Survey (APASS), funded by the for Solar System Studies: L4 Greek Camp and Spies.” Minor Robert Martin Ayers Sciences Fund. The purchase of a FLI- Planet Bul. 43, 323-331. 1001E CCD cameras was made possible by a 2013 Gene Shoemaker NEO Grants from the Planetary Society. Minor Planet Bulletin 44 (2017) 316

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid G., Prince, T.A., Kulkarni, S. (2015). “Asteroid lightcurves from Lightcurve Database.” Icarus 202, 134-146. Updated 2017 April. the Palomar Transient Factory survey: Rotation periods and phase http://www.minorplanet.info/lightcurvedatabase.html functions from sparse photometry.” Astron. J. 150, A75.

Waszczak, A., Chang, C., Ofek, E.O., Laher, R., Masci, F., Levitan, D., Surace, J., Cheng, Y., Ip, W., Kinoshita, D., Helou,

ROTATION PERIOD DETERMINATION FOR 397 VIENNA Observations on 12 nights 2017 May 10 – June 18 provide a good fit to an irregular lightcurve with period 15.461 ± 0.001 hours, Frederick Pilcher amplitude 0.16 ± 0.02 magnitudes. This is consistent with Organ Mesa Observatory (MPC G50) previous measurements. 4438 Organ Mesa Loop Las Cruces, NM 88011 USA References [email protected] Behrend, R. (2009). Observatoire de Geneve web site. A. Marciniak, K. Kaminski, J. Horbowicz, J. Skrzypek http://obswww.unige.ch/~behrend/page_cou.html. Astronomical Observatory Institute Faculty of Physics Harris, A.W., Young, J.W. (1980). “Asteroid Rotation IV.” A. Mickiewicz University Icarus 54, 59-109 Sloneczna 36 60-286 Poznan, POLAND Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and Julian Oey 444 Gyptis.” Icarus 57, 251-258. Blue Mountain Observatory (MPC Q68) 94 Rawson Pde. Leura, NSW, AUSTRALIA Ruthroff, J. C. (2010). “Photometric observations and lightcurve analysis of asteroids 397 Vienna and (5153) 1940 GO.” Minor W. Ogloza Planet Bull. 37, 32-33. Mt. Suhora Observatory, Pedagogical University Podchorazych 2, 30-084 Cracow, POLAND

(Received: 2017 June 14)

CCD photometry of minor planet 397 Vienna shows that it has a synodic rotation period of 15.461 ± 0.001 hours, amplitude 0.16 ± 0.02 magnitudes.

Previously published periods for 397 Vienna were reported by Harris and Young (1983), 15.48 hours; Behrend (2009), >8 hours; and Ruthroff (2010), 15.45 hours. The authors of this study agreed to collaborate to obtain a dense observation set and complete phase coverage.

Observer Pilcher at the Organ Mesa Observatory used a 0.35- meter Meade LX200 GPS Schmidt-Cassegrain (SCT), SBIG STL- 1001E CCD, clear filter (sessions 2619, 2632, 2636, 2643, 2653, 2655). Oey at Blue Mountain Observatory used a 35 cm SCT operating at f/5.9, SBIG ST-8XME CCD, clear filter (sessions 2657, 2658). The staff of A. Mickiewicz University obtained data at Borowiec station with 0.4 meter Newtonian telescope, SBIG ST7 CCD, clear filter (sessions 2644, 2645), and at Winer Observatory near Sonoita, Arizona, USA with a 0.7 meter corrected Dall-Kirkham telescope, Andor iXon CCD, R filter (session 2646). Ogloza at Mt. Suhora Observatory used a 0.6 meter Cassegrain, Apogee Alta U47 CCD, R filter (session 2661). Photometric measurement and lightcurve construction are with MPO Canopus software. To reduce the number of points on the lightcurves and make them easier to read, data points have been binned in sets of 3 with a maximum time difference of 5 minutes.

Number Name 2017/mm/dd Pts Phase LPAB BPAB Period(h) P.E Amp A.E. 397 Vienna 05/10-06/18 1786 10.3, 5.2, 7.3 253 6 15.461 0.001 0.16 0.02 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first date, minimum (second) value reached, and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Minor Planet Bulletin 44 (2017) 317

LIGHTCURVES OF 131 VALA AND 612 VERONIKA DURING THEIR 2017 APPARITIONS

Frederick Pilcher Organ Mesa Observatory (G50) 4438 Organ Mesa Loop Las Cruces, NM 88011 USA [email protected]

(Received: 2017 July 2)

Synodic rotation periods and amplitudes are found for 131 Vala 5.1802 ± 0.0002 hours, 0.08 ± 0.01 magnitudes; and for 612 Veronika 8.243 ± 0.001 hours, 0.09 ± 0.01 magnitudes.

Observations to obtain the data used in this paper were made at the Organ Mesa Observatory with a 0.35-meter Meade LX200 GPS Schmidt-Cassegrain (SCT) and SBIG STL-1001E CCD. Exposures were 60 seconds, unguided, with a clear filter. Photometric measurement and lightcurve construction is with MPO Canopus software. To reduce the number of points on the lightcurves and make them easier to read, data points have been binned in sets of 3 with a maximum time difference of 5 minutes.

131 Vala. Pilcher (2008) published a highly symmetrical bimodal lightcurve of 131 Vala with period 10.359 hours, amplitude 0.09 magnitudes based on observations in 2007 October-November near celestial longitude 45 degrees. Parallel studies near the next opposition 2009 February-April near celestial longitude 200 degrees by Behrend (2009), Galad (2010), and Pilcher (2009) all produced bimodal lightcurves with a good fit to periods near 5.181 hours and amplitudes near 0.25 magnitudes. Pilcher (2009) replotted his year 2007 observations to a monomodal lightcurve with period 5.179 hours. New observations on 4 nights 2017 May 13 – June 15 near celestial longitude 230 degrees, almost directly opposite in the sky to the 2007 observations, provide a good fit to a monomodal lightcurve with period 5.1802 ± 0.0002 hours, amplitude 0.08 ± 0.01 magnitudes. This is in excellent agreement 612 Veronika. Parallel studies by Pilcher (2013), and by Strabla et with earlier studies. A split halves plot of the double period shows al. (2013) obtained periods of 8.243 hours and 8.244 hours that the two halves are identical within reasonable photometric respectively, and almost identical lightcurves, based on error, and a period spectrum is also presented. observations 2012 August – October. New observations on 7 nights 2017 May 24 – July 1 are in complete agreement, providing a good fit to an irregular lightcurve with period 8.243 ± 0.001 hours, amplitude 0.09 ± 0.01 magnitudes. A period spectrum rules out all other periods except for the double period, and a split halves plot shows that the two halves of the double period are identical within reasonable photometric error.

Minor Planet Bulletin 44 (2017) 318

Number Name 2017/mm/dd Pts Phase LPAB BPAB Period(h) P.E Amp A.E.

131 Vala 05/13-06/15 882 1.8, 16.9 230 1 5.1802 0.0002 0.08 0.01 612 Veronika 05/24-07/01 1521 10.4, 10.2, 14.3 255 22 8.243 0.001 0.09 0.01 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date, unless a minimum (second value) was reached. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

References

Behrend, R. (2009). Observatoire de Geneve web site. http://obswww.unige.ch/~behrend/page_cou.html.

Galad, A., Kornos, L., Vilagi, J. (2010). “An ensemble of lightcurves from Modra.” Minor Planet Bull. 37, 9-15.

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Pilcher, F. (2008). “Period determinations for 84 Klio, 98 Ianthe, 102 Miriam, 112 Iphigenia, 131 Vala, and 650 Amalasuntha.” Minor Planet Bull. 35, 71-72.

Pilcher, F. (2009). “Rotation period determinations for 120 Lachesis, 131 Vala, 157 Dejanira, and 271 Penthesilea.” Minor Planet Bull. 36, 100-102.

Strabla, L., Quadri, U., Girelli, R. (2013). “Asteroids observed from Bassano Bresciano Observatory 2012 August-December.” Minor Planet Bull. 40, 83-84.

Minor Planet Bulletin 44 (2017) 319 (24495) 2001 AV1 – A SUSPECTED VERY WIDE BINARY

Robert D. Stephens Center for Solar System Studies (CS3) / MoreData! 11355 Mount Johnson Ct. Rancho Cucamonga, CA 91737 USA [email protected]

Brian D. Warner Center for Solar System Studies – Palmer Divide Station Eaton, CO USA

Amadeo Aznar Macias Issac Aznar Observatory (Z95) Valencia, SPAIN

Vladimir Benishek Sopot Astronomical Observatory (K90) Sopot, SERBIA

(Received: 2017 July 7)

We report that asteroid (24495) 2001 AV1 is a binary asteroid. It is another candidate for the special case of very wide binaries. The primary lightcurve has a period of 24.083 ± 0.005 h and an amplitude 0.58 ± 0.05 mag. and the secondary lightcurve has a period of 2.7375 ± 0.0001 h.

The Mars crosser (24495) 2001 AV1 was initially observed by Stephens using a 0.40-m Schmidt-Cassegrain telescope with Finger Lakes ProLine ML-1001E CCD camera from the Center for Solar System Studies (U82) located in Landers California.

The analysis of the first few sessions showed the signature of From the angle of the slope of the ascension and the lack of a clear another possible candidate for a special case of very wide binaries extrema in any session, it appeared the main dominant, primary (see Jacobson et al., 2014, Warner 2016). This is where the period was close to a multiple of the Earth’s rotation with the most primary period belonging to the main body is long with a large likely period being near 48 h. amplitude and the secondary period is short with a low amplitude. For wide binaries, the chance of observing a mutual event (eclipse A call for observations were made to several observers located in or occultation) would be very rare because of the long primary Europe, about 110°-150° in longitude from the CS3 observatories period. In the case of (24495) 2001 AV1, each of the first sessions in California. Aznar from his observatory in Valencia, Spain was showed a trend of brightening over the course of the night with a able to observe the asteroid on several nights. Benishek observed secondary frequency less than three hours superimposed on the the asteroid two nights overlapping Aznar’s data. Table 1 gives the upward trend. telescopes and CCD cameras used for observations. Exposures were unfiltered and ranged from 240 to 300 seconds. Table II gives the dates and session numbers in the lightcurves for each observer.

The raw images were flat-field and dark subtracted before being measured in MPO Canopus. Night-to-night linkage was aided by the Comp Star Selector utility which helps find near-solar color comparison stars, thus reducing color difference issues. Stars were chosen from the CMC-15 catalog (http://svo2.cab.inta- csic.es/vocats/cmc15/). Generally, needed zero points adjustments are within ±0.05 of one another, but larger adjustments can be required to minimize the RMS value from the Fourier analysis.

Observer Telescope Camera Stephens 0.40m SCT FLI Proline 1001E Aznar 0.35m SCT SBIG STL-1001E Benishek 0.35m SCT SBIG ST-8X ME

Table I. List of observers and equipment. SCT: Schmidt- Cassegrain.

Minor Planet Bulletin 44 (2017) 320

Observer Telescope Sess Stephens 0.40m SCT 1,2,3,4,5,6,7,8,9, 11,13,15,16,19,23 Aznar 0.35m SCT 10,12,14,17,18,21 Benishek 0.35m SCT 20,22

Table II. List of observation and session numbers in the lightcurves for each observer.

Period Analysis

Period analysis was done using MPO Canopus, which employs the FALC Fourier analysis algorithm developed by Harris (Harris et al., 1989). MPO Canopus can do a dual-period search process. The program first finds an initial value for the dominant (usually shorter) period. The Fourier model lightcurve is subtracted from the data set in the succeeding search for a second period. The Fourier curve for that second period is then subtracted from the Conclusion data set in a new search for the dominant period. The iterative process continues until both periods stabilize and it produces Because the primary period is so close to an Earth day, it was not reasonable lightcurves. possible to get a complete lightcurve for P1. This asteroid should be a prime target for follow up at its next opposition in January 2020 when the northern hemisphere nights will be much longer.

Acknowledgements

Work on the asteroid lightcurve database (LCDB) was also funded in part by National Science Foundation grant AST-1507535. The purchase of the FLI-1001E CCD camera was made possible by a 2013 Gene Shoemaker NEO Grant from the Planetary Society.

References

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., The dual period analysis found a primary lightcurve belonging to Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, the main body of P1 = 24.083 ± 0.005 h, A1 = 0.50 ± 0.02 mag H., Zeigler, K.W. (1989). “Photoelectric Observations of (“P1” plot). Assuming an equatorial view of the asteroid, this Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. leads to an a/b ratio of the asteroid’s silhouette of 1.6:1. As expected, subtracting this lightcurve from the data set and doing a Jacobson, S.A., Scheeres, D.J., McMahon, J. (2014). “Formation period search found a solution that showed no mutual events of the Wide Asynchronous Binary Asteroid Population.” Ap. J. (occultations and/or eclipses) due to a satellite (“P2” plot). The 780:60. lightcurve has a period of P2 = 2.7375 ± 0.0001 h, A2 = 0.19 mag. In the case of a Very Wide Binary, the larger amplitude is Warner, B.D. (2007). “Initial Results of a Dedicated H-G assumed to be for the main body. “The amplitude of the longer Program.” Minor Planet Bul. 34, 113-119. period if it were due to the secondary with about a magnitude of Warner, B.D. (2016). “Three Additional Candidates for the Group "dilution" from the primary, it would have to have an unphysically of Very Wide Binaries.” Minor Planet Bul. 43, 306-309. great elongation plus being viewed almost exactly equatorially in order to produce the "diluted" amplitude that large. The inferred Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid size ratio comes from the secondary having extracted almost all of Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Feb. the angular momentum of the primary spin but not quite http://www.minorplanet.info/lightcurvedatabase.html escaping.” (Harris private communication).

Number Name mm\dd Pts Phase LPAB BPAB Period P.E. Amp A.E. 24495 2001 AV1 05/03-05/19 82043 198 3624.083 0.0050.50 0.02 2.7375 0.00010.19 0.02 Table III. Observing circumstances and results. Pts is the number of data points. Grp is the asteroid family/group (Warner et al., 2009). The first line is the primary (P1) period and the second line is the secondary (P2) period.

Minor Planet Bulletin 44 (2017) 321

ASTEROIDS OBSERVED FROM CS3: 1696 Nurmela. The rotational period for this Vestoid has been 2017 APRIL - JUNE found twice in the past (Stephens et al. 2007 and Galad et al. 2008). Both sets of prior observations were obtained within a few Robert D. Stephens weeks of each other. The result found this year is in good Center for Solar System Studies (CS3)/MoreData! agreement with those findings. 11355 Mount Johnson Ct., Rancho Cucamonga, CA 91737 USA [email protected]

(Received: 2017 July 7)

CCD photometric observations of 11 main-belt asteroids were obtained from the Center for Solar System Studies from 2017 April to June.

The Center for Solar System Studies “Trojan Station” (CS3, MPC U81) has two telescopes which are normally used in program asteroid family studies. During the 2nd quarter of 2017 the Jovian Trojans which are normally studied were out of season, so targets of opportunity amongst the Main Belt families were selected.

All images were made with a 0.4-m or a 0.35-m SCT using an FLI ML-Proline 1001E or FLI ML-Microline 1001E CCD camera. Images were unbinned with no filter and had master flats and 1998 Titius. The period found this year agrees with our previous darks applied. Image processing, measurement, and period finding of 6.13 h (Stephens 2002). analysis were done using MPO Canopus (Bdw Publishing), which incorporates the Fourier analysis algorithm (FALC) developed by Harris (Harris et al., 1989). Night-to-night calibration (generally < ±0.05 mag) was done using field stars from the CMC-15 catalog or APASS (Henden et al., 2009) The Comp Star Selector feature in MPO Canopus was used to limit the comparison stars to near solar color.

In the lightcurve plots, the “Reduced Magnitude” is Johnson V corrected to a unity distance by applying -5*log (r∆) to the measured sky magnitudes with r and ∆ being, respectively, the Sun-asteroid and the Earth-asteroid distances in AU. The magnitudes were normalized to the phase angle given in parentheses using G = 0.15. The X-axis rotational phase ranges from -0.05 to 1.05.

The amplitude indicated in the plots is the amplitude of the Fourier model curve and not necessarily the adopted amplitude of the lightcurve. 2572 Annschnell. This Vestoid had its rotational period determined once before (Behrend 2006). The result found this year 1369 Ostanina. The rotational period for this Outer Main Belt is in good agreement with that result. asteroid has been determined several times in the past. Chiorny (2007), Behrend (2006, 2011, 2012, and 2016) each reported a rotational period near 8.4 h. The result from this opposition is in good agreement with those results.

3193 Elliot. No entry for this Vestoid could be found in the Lightcurve Database (Warner et al. 2009). Minor Planet Bulletin 44 (2017) 322

4008 Corbin. Parvec (2017) reported a rotational period of 6.203 h 6921 Janejacobs. No entry for this Vestoid could be found in the from the Photometric Survey for Asynchronous Binary Asteroids. Lightcurve Database (Warner et al. 2009). This result agrees with that determination.

7247 Robertstirling. Warner (2013a, 2014b) determined a 4464 Vulcano. Warner (2011, 2014a, 2016) observed this rotational period for this Hungaria twice in the past both times Hungaria several times in the past finding rotational periods near with a rotational period near 3.18 h. This year’s result agrees with 3.2 h. those past findings.

6107 Osterbrock. Warner (2012, 2014a) previously reported (13186) 1996 UM. Warner observed this Hungaria three times in periods of 2.372 h and 2.215 h, each with an amplitude under 0.1 the past (Warner 2013b, 2014b and 2016) each time finding a mag. and multiple extrema using observations spanning 3 or 4 period near 4.3 h. This year’s results agree with those findings. nights. No signature for these shorter periods could be found in this dataset and the rotational period of 39.24 h could not be reconciled to the previous results.

Minor Planet Bulletin 44 (2017) 323

Warner, B.D. (2011). “Lightcurve Analysis of Hungaria Asteroid 4464 Vulcano.” Minor Planet Bul. 38, 168-169.

Warner, B.D. (2012). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2012 March – June.” Minor Planet Bul. 39, 168-169.

Warner, B.D. (2013a). “Rounding Up the Unusual Suspects.” Minor Planet Bul. 40, 36-42.

Warner, B.D. (2013b). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2012 June - September.” Minor Planet Bul. 40, 26-29.

Warner, B.D. (2014a). “Asteroid Lightcurve Analysis at CS3- Palmer Divide Station: 2014 January-March.” Minor Planet Bul. 41, 245-252. Acknowledgements Warner, B.D. (2014b). “Asteroid Lightcurve Analysis at CS3- This research was made possible in part based on data from Palmer Divide Station: 2014 March-June.” Minor Planet Bul. 41, CMC15 Data Access Service at CAB (INTA-CSIC) 235-241. (http://svo2.cab.inta-csic.es/vocats/cmc15/). The purchase of a Warner, B.D. (2016). “Asteroid Lightcurve Analysis at the Palmer FLI-1001E CCD cameras was made possible by a 2013 Gene Divide Observatory: 2015 June-September.” Minor Planet Bul. 43, Shoemaker NEO Grants from the Planetary Society. 57-65. References Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Galad, A., Kornos, L. (2008). “A Sample of Lightcurves from Lightcurve Database.” Icarus 202, 134-146. Updated 2017 Apr. Modra.” Minor Planet Bul. 35, 78-81. http://www.minorplanet.info/lightcurvedatabase.html

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Pravec, P. (2017). Photometric Survey for Asynchronous Binary Asteroids web site. http://www.asu.cas.cz/~asteroid/binastphotsurvey.htm.

Stephens, R.D. (2002). “Photometry of 973 Aralia, 1189 Terentia, 1040 Klumpkea, and 1998 Titius.” Minor Planet Bul. 29, 47-48.

Stephens, R.D., Malcolm, G. (2007). “Lightcurve Analysis of 1489 Attila and 1696 Nurmela.” Minor Planet Bul. 34, 78.

Number Name mm\dd Pts Phase LPAB BPAB Period P.E. Amp A.E. Grp 1369 Ostanina 06/09-06/12 167 18.8,18.1 298 17 8.399 0.004 0.96 0.02 MB-O 1696 Nurmela 04/09-04/12 163 27.1,27.6 144 5 3.159 0.001 0.58 0.02 V 1998 Titius 04/09-04/12 163 19.1,20.0 159 1 6.133 0.004 0.24 0.02 V 2572 Annschnell 06/08-06/11 122 21.5,22.5 221 4 6.343 0.003 0.82 0.02 V 3193 Elliot 04/23-05/03 213 15.3,18.7 184 0 3.103 0.001 0.18 0.03 V 4008 Corbin 05/09-05/18 185 28.6,29.4 173 11 6.180 0.004 0.23 0.02 PHO 4464 Vulcano 04/13-04/16 196 6.4,8.3 194 -3 3.209 0.002 0.10 0.02 H 6107 Osterbrock 06/12-06/29 380 34.3,35.2 215 30 39.24 0.03 0.24 0.03 H 6921 Janejacobs 04/29-05/02 161 3.3,4.0 217 6 5.062 0.001 1.20 0.02 V 7247 Robertstirling 06/04-06/07 180 18.5,18.6 257 30 3.17 0.01 0.14 0.02 H 13186 1996 UM 05/04-05/05 123 10.7,10.9 222 17 4.304 0.004 0.34 0.02 H Table I. Observing circumstances and results. Pts is the number of data points. The phase angle values are for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009).

Minor Planet Bulletin 44 (2017) 324

LIGHTCURVE ANALYSIS OF NEA (190166) 2005 UP156: A NEW FULLY-SYNCHRONOUS BINARY

Brian D. Warner Center for Solar System Studies–Palmer Divide Station 446 Sycamore Ave. Eaton, CO 80615 USA [email protected]

Alan W. Harris MoreData! La Cañada, CA USA

Amadeo Aznar Macías APT Observatory Group EURONEAR SPAIN Soon after the discovery announcement, Aznar and Oey provided Julian Oey data to Warner to try to improve lightcurve and event coverage as Blue Mountains Observatory (MPC Q68) well as the orbital/rotational period. Table II shows the Leura, NSW, AUSTRALIA instrumentation used during the campaign.

(Received: 2017 July 7) OBS Telescope Camera Warner 0.30-m f/9.6 SCT FLI ML-1001E CCD photometric observations of the near-Earth Aznar 0.35-m f/10 SCT SBIG STL-1001E asteroid (190166) 2005 UP156 in 2017 May show it to Oey 0.35-m f/11 SCT Apogee U6M be a fully-synchronous binary with rotation and orbital period P = 40.542 ± 0.008 h. The estimated effective Table II. List of observers and equipment. diameter ratio of the two bodies is 0.8 ± 0.1. However, the 0.5 mag out-of-eclipse lightcurve indicates quite elongated shapes and so the size ratio should be viewed with caution.

The near-Earth asteroid (190166) 2005 UP156 was observed by Warner in 2014 (Warner, 2015) who found a period of 40.5 h and amplitude of 0.79 mag. Based on a relatively sparse data set, there were no indications of the asteroid being other than a single, highly-elongated body. Those observations were made at about 43° solar phase angle and phase angle bisector longitude of 5° (see Harris et al., 1984).

Warner began observing the asteroid during the 2017 apparition on May 4. By May 19, there was clear evidence that the asteroid was a fully-synchronous binary, i.e., two bodies in close proximity with the rotation period of each body the same as the orbital period. After the observations on May 23, the lightcurve was sufficiently covered to determine the period and approximate size ratio of the bodies. At that time Warner and Harris (2017) submitted a CBET that was published shortly afterwards.

They reported an orbital/rotation period of 40.542 ± 0.008 h and total lightcurve amplitude of 1.1 mag. the out-of-eclipse lightcurve showed an amplitude of 0.5 mag with the eclipse events being about 0.6 mag. Using the latter value gives an effective diameter ratio of the two bodies of 0.8 ± 0.1. This should be considered only a first approximation since the large amplitude of the out-of- eclipse lightcurve indicates that the individual bodies are quite elongated.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 190166 2005 UP156 05/04-06/12 1585 10.8,28.2 230-252 6-16 48.6 0.1 0.12 0.01

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude over the range of dates (see Harris et al., 1984).

Minor Planet Bulletin 44 (2017) 325

Additional observations by all observers provided the opportunity LIGHTCURVE ANALYSIS OF THE to follow changes in the lightcurve. For example, in the few days NEAR-EARTH ASTEROID 6063 JASON after the initial lightcurve, the “shoulders,” sharp changes in the lightcurve slope, became more apparent. These gave further Brian D. Warner evidence of the binary nature of the asteroid. Note that the depths Center for Solar System Studies–Palmer Divide Station of the two events were almost identical. 446 Sycamore Ave. Eaton, CO 80615 USA A third lightcurve, including data from May 29 to June 12 also [email protected] shows shoulders, more so at the second event around 0.7 rotation phase. More so, the depth of the two events was no longer Amadeo Aznar Macías symmetrical. The full effect of the lightcurve changes is seen APT Observatory Group when trying to find a single period using the entire data set. EURONEAR SPAIN

Vladimir Benishek Sopot Astronomical Observatory (K90) Sopot, SERBIA

Julian Oey Blue Mountains Observatory (MPC Q68) Leura, NSW, AUSTRALIA

Roger Groom Darling Range Observatory Perth, WA, AUSTRALIA

(Received: 2017 July 7) Going Deeper into the Analysis CCD photometric observations of the near-Earth The 40.6 hour orbit period implies that the two components, if asteroid 6063 Jason were made in 2017 June. A equal spheres of density ~2.5 gm/cm3, would have an orbit radius collaboration of five observers at widely-separated about 9 times the radius of the two bodies. Since the non-eclipse longitudes proved critical in finding a synodic period of amplitude of the lightcurve implies nearly 2:1 elongation of the 48.6 h, nearly commensurate with an Earth day, and bodies, the separation may be more like 6 times the long semi- confirming that the asteroid is most likely tumbling. axis, but the short semi-axis profiles would be closer to 1/12 of the separation (or full-width ratio about 1/6). This geometrical Previous data for near-Earth asteroid 6063 Jason indicated it may proportion is approximately confirmed by the width of the eclipse be a low amplitude non-principal axis rotation (“tumbler”; Petr events, which are only about 0.05 rotation phase wide. A Pravec, private communications, 2013). Using data from Warner consequence of the narrowness of the events is that events will (2014), Pravec found a strong signal for a period at about 51.3 h. only be seen within about ten degrees of equatorial aspect, thus He also found a secondary period of 238 h, but it was not possible not seeing eclipse events at other apparitions is not surprising. to find a definitive answer. Acknowledgements Renewed CCD photometric observations of the asteroid were Work on the asteroid lightcurve database (LCDB) is funded by made by the authors in 2017 June. Table I gives the equipment National Science Foundation grant AST-1507535. used. The hope was to confirm and improve the earlier results.

References OBS Telescope Camera Warner 0.30-m f/9.6 SCT FLI ML-1001E Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). Aznar 0.35-m f/10 SCT SBIG STL-1001E “Lightcurves and phase relations of the asteroids 82 Alkmene and Benishek 0.35-m f/10 SCT SBIG ST-8XME 444 Gyptis.” Icarus 57, 251-258. Oey 0.35-m f/11 SCT Apogee U6M Groom 0.30-m f/7.2 SCT SBIG ST-8XME Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, T.C., Welch, D.L. (2009). http://www.aavso.org/apass Table I. List of observers and equipment. All observers used MPO Canopus to measure images, taking Warner, B.D. (2015). “Near-Earth Asteroid Lightcurve Analysis at advantage of the Comp Star Selector utility to find near solar-color CS3-Palmer Divide Station: 2014 June-October.” Minor Planet stars for ensemble differential photometry. The V magnitudes of Bull. 42, 41-53. stars from the APASS catalog (Henden et al., 2009) were used for Warner, B.D., Harris, A.W. (2017). “(90166) 2005 UP156.” CBET the reductions. 4394. The initial observations by Warner (Jun 13-18) indicated the possibility of a longer period, just as was seen in the 2013 apparition. In that earlier work, it was obvious that data from a single station alone could not find an answer and so the collaboration of the five authors was formed.

Minor Planet Bulletin 44 (2017) 326

Based on the data set that spanned more than two weeks and this period is in reasonable agreement with the one from 2013. leaving the nightly zero points almost untouched (adjustments <0.05 mag), even the raw plot, i.e., magnitude vs. JD without fitting to a period, showed a sinusoidal curve that apparently confirmed a long period component. Assuming a bimodal shape, analysis of the data set showed a period of about 680 h, which was much longer than the previously reported long period. However, that previous result was just one many possible solutions based on data from one location.

As it turns out, because of the low-level tumbling action, the dual- period search in MPO Canopus found nearly identical results for the “short” period. This is rarely the case, and never when the periods are very short and/or the tumbling is in a very excited state. However, this does point to the need for caution in interpreting the analysis. As mentioned previously, the analysis also led to the false conclusion that they system was a special type An email query to radar observers got a response from Ellen of binary. Howell (private communications) who had also worked the asteroid in 2013 as well as the 2017 apparition. She said there Unfortunately, because of the long periods, even with a good were no obvious indications of the long period, originally network of observers, it may never be possible to find the true suspected by Warner to be one component of a very wide binary parameters of the system, unless the combination of radar and asteroid. She did, however, confirm a dominant period of about 48 optical data might do so. Often the best possible result in cases hours based on radar images and other data. such as this is to be able to use only descriptive terms: “With reasonable certainty, the asteroid is a tumbler with long periods.”

Acknowledgements

Work on the asteroid lightcurve database (LCDB) is funded by National Science Foundation grant AST-1507535. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. (http://www.ipac.caltech.edu/2mass/)

References MPO Canopus is not capable of analyzing tumbling asteroids; it can do dual-period searches only when the two periods are Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). additive, such as happens with a binary asteroid. However, “Lightcurves and phase relations of the asteroids 82 Alkmene and because the tumbling is thought to be low-level with very long 444 Gyptis.” Icarus 57, 251-258. periods, we attempted to find a dominant period by using a search to a range of 10-70 hours and then forcing the nightly zero points Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, to get a best Fourier fit, favoring one near 50 hours in case of any T.C., Welch, D.L. (2009). http://www.aavso.org/apass ambiguities. Warner, B.D. (2014). “Near-Earth Asteroid Lightcurve Analysis a The period spectrum shows several noticeable minimum points, all CS3-Palmer Divide Station: 2013 September-December.” Minor nearly commensurate with an Earth day. This alone made it Planet Bull. 41, 113-124. imperative to have data from widely-separated longitudes. The final result was a period of 48.6 ± 0.1 h with an amplitude of 0.12 mag. Given the uncertainties in the results from 2013 and 2017,

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 6063 Jason 06/13-06/26 1208 32.3,28.6 247 13 48.6 0.1 0.12 0.01

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

Minor Planet Bulletin 44 (2017) 327

LIGHTCURVE ANALYSIS OF In the plots below, the “Reduced Magnitude” is Johnson V as TWO NEAR-EARTH ASTEROIDS: indicated in the Y-axis title. These are values that have been 2010 VB1 AND 2014 JO25 converted from sky magnitudes to unity distance by applying –5*log (rΔ) to the measured sky magnitudes with r and Δ being, Brian D. Warner respectively, the Sun-asteroid and Earth-asteroid distances in AU. Center for Solar System Studies / MoreData! The magnitudes were normalized to the given phase angle, e.g., 446 Sycamore Ave. alpha(6.5°), using G = 0.15, unless otherwise stated. The X-axis is Eaton, CO 80615 USA the rotational phase, ranging from –0.05 to +1.05. [email protected] If the plot includes an amplitude, e.g., “Amp: 0.65”, this is the (Received: 2017 July 7) amplitude of the Fourier model curve and not necessarily the adopted amplitude for the lightcurve. The value is provided as a CCD photometric observations were made of the near- matter of convenience. Earth asteroids (NEAs) 2010 VB1 in 2017 June and 2014 JO25 in 2017 April. The lightcurves for both 2010 VB1. This NEA made its closest approach in 2017 June. The asteroids showed significant day-to-day evolution due to exposures on June 19 and 20 were only 20 seconds. This was changing viewing aspects. For 2010 VB1, the average because 1) of the asteroid’s rapid sky motion and 2) given its synodic period was 0.18919 ± 0.0002 h while the estimated size of only 70 meters, the possibility that its rotation amplitude decreased in near step with the phase angle, period could be on the order of only a few minutes. Pravec et al. going from 0.99 mag at 54° to 0.61 mag at 27°. For (2000) showed that exposures can be no longer than about 0.187x 2014 JO25, the average synodic period was 4.60 ± the period. Otherwise, “rotational smearing” occurs, meaning that 0.04 h. Its amplitude ranged from 0.39 to 0.14 mag. details of the lightcurve are lost since the single observation covers too much of a rotation. Because of the rapid sky motion, up to five “sessions” were required, i.e., five different sets of The somewhat close flybys of the near-Earth asteroids 2010 VB1 comparison stars were used. and 2014 JO25 in 2017 provided a good opportunity to study their lightcurve evolution as the viewing aspects (phase angle and phase angle bisector) changed by significant amounts.

Desig Telescope Camera Squirt 0.30-m f/6.3 Schmidt-Cass ML-1001E Borealis 0.35-m f/9.1 Schmidt-Cass FLI-1001E Table I. List of CS3-PDS telescope/CCD camera combinations.

Table I gives the telescope-camera combinations used for the two campaigns conducted at CS3-PDS. All observations were unfiltered since a clear filter can result in a 0.1-0.3 magnitude loss. The exposure duration varied depending on the asteroid’s brightness and sky motion. If necessary, an elliptical aperture with the long axis parallel to the asteroid’s path was used.

Measurements were made using MPO Canopus. The Comp Star Selector utility in MPO Canopus found up to five comparison The plot above shows the raw data from just one session on June stars of near solar-color for differential photometry. Catalog 19. At first glance, it appears to be useless data because of large magnitudes were usually taken from the CMC-15 scatter. However, because of the possible super-fast rotation, a (http://svo2.cab.inta-csic.es/vocats/cmc15/) or APASS (Henden et period search was run from 0.001 to 1.500 h in steps of al., 2009) catalogs. Period analysis is also done with MPO 0.001 h using all the data from that night. The result was a dense, Canopus, which implements the FALC algorithm developed by well-defined bimodal lightcurve with a period of 0.18908 ± Harris (Harris et al., 1989). 0.00004 h and amplitude of about 0.98 mag.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period (h) P.E. Amp A.E. 2010 VB1 06/19 481 53.4 245 17 0.18908 0.00004 0.98 0.05 06/20 250 46.9 249 15 0.18912 0.00005 0.81 0.03 06/21 357 41.5 251 13 0.18920 0.00005 0.83 0.03 06/22 136 37.2 254 11 0.1891 0.0001 0.67 0.03 06/23 217 33.8 256 9 0.18895 0.00005 0.63 0.03 06/24 47 31.1 257 8 0.1895 0.0004 0.70 0.05 06/25 148 29.0 259 7 0.18915 0.00008 0.62 0.03 06/26 51 27.3 261 6 0.1894 0.0002 0.61 0.03 2014 JO25 04/20 328 38.3,30.6 197 12 4.64 0.01 0.21 0.01 04/21 265 24.7,24.2 198 3 4.53 0.02 0.39 0.03 04/22-04/24 473 23.9,25.1 201 -6 4.561 0.007 0.14 0.01

Table II. Observing circumstances. Pts is the number of data points used in the analysis. The phase angle (α) and phase angle bisector longitude (L) and latitude (B) are the average values for the given date or date range.

Minor Planet Bulletin 44 (2017) 328

As the asteroid retreated from the Earth’s neighborhood and the sky motion decreased, exposures were gradually lengthened to keep the signal-to-noise as high as possible. From June 22-25, 40 second exposures were used while for June 26 exposures were extended to 120 seconds. In all 1687 data points were acquired over the eight consecutive nights of observations.

The lightcurves below go from June 19-26 and show how the shape and amplitude evolved as the phase angle decreased from about 54° to 28°. The biggest change is the decreasing depth of the second minimum at about 0.75 rotation phase.

The final plot in the set shows the amplitude versus phase angle. As expected, the amplitude decreased along with the phase angle (Zappala et al., 1990). From the trend line alone, the amplitude would be about 0.28 mag at 0° phase angle. That should be taken with a healthy dose of skepticism since the shadowing effects (or lack of them) at near 0° phase angle could easily change things.

Minor Planet Bulletin 44 (2017) 329

bimodal solution up to an amplitude of about 0.37 mag. Since this was a known to be a target for the radar team, an email was sent to them to see if their observations supported the shortest period. They did not (Patrick Taylor, private communications), but instead favored a period of about 4.5 hours.

2014 JO25. This NEA made its closest approach in mid-April 2017 when it was the target of radar and optical observations. The first observations at PDS were made on April 20. Here again, due to rapid sky motion, exposures were very short, only 5 seconds. The longer period was adopted, resulting the in second lightcurve Fortunately, the asteroid was V ~ 10.5 and so a reasonable SNR for April 20, and for period searches on subsequent days. was obtained. Exposures on April 21 were 10 seconds and increased to 30 seconds for April 22-24. Unlike for 2010 VB1, the The lightcurve for April 21 remains a mystery. Measuring the estimated size of 2014 JO25 (D ~ 860 m) was well above the limit images required using several sets of comp stars. To help assure where a superfast rotator might be expected. good session-to-session zero point alignment, the last 5-10 images of a given session were remeasured for the following session. This should have led to 5-10 data overlapping data points in the raw plot. Slight adjustments (usually <0.05 mag) were required to get the best overlapping fit between the two sessions. This process was repeated for each subsequent session. Despite this, the lightcurve was dramatically different in shape and amplitude from the night before. The same algorithm to correct for changing phase angle and viewing aspect was used throughout, so it would be strange that this lightcurve would be so different. The possible, maybe even probable, cause is the shape of the asteroid, which was found by radar to be a double-lobed (highly bifurcated) body, along with a different viewing aspect.

There are some excellent radar image animations available of this asteroid, for example,

https://www.youtube.com/watch?v=usPrwjyggEM The initial analysis of the April 20 data showed three likely periods: about 3, 4.5, and 6 hours, the second and third periods being 1.5x and 2x the shortest period. A bimodal lightcurve is typically the correct solution when the amplitude is about 0.2 mag and greater, but – in truth – Harris et al. (2014) allow for a non-

Minor Planet Bulletin 44 (2017) 330

Acknowledgements

Funding for PDS observations, analysis, and publication was provided by NASA grant NNX13AP56G. Work on the asteroid lightcurve database (LCDB) was also funded in part by National Science Foundation grant AST-1507535. This research was made possible in part based on data from CMC15 Data Access Service at CAB (INTA-CSIC) (http://svo2.cab.inta-csic.es/vocats/cmc15/) and the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund.

References

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258. As the asteroid receded on April 22-24, the phase angle and viewing aspects did not change by large amounts. Given this and Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., an assumed spin axis alignment that meant a similar silhouette was Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, seen each night, the lightcurve returned to a low amplitude shape H., Zeigler, K.W. (1989). “Photoelectric Observations of that was then bimodal when keeping the period near 4.5 h. Despite Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. only small changes in viewing aspect and phase angles, there are still signs of slight changes in the lightcurve. Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., Vilagi, J., Gajdos, S., Carbognani, A., Hornoch, K., Kusnirak, P., Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B.W. (2014). “On the maximum amplitude of harmonics on an asteroid lightcurve.” Icarus 235, 55-59.

Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, T.C., Welch, D.L. (2009). http://www.aavso.org/apass

Pravec, P., Hergenrother, C., Whiteley, R., Sarounova, L., Kusnirak, P. (2000). “Fast Rotating Asteroids 1999 TY2, 1999 SF10, and 1998 WB2.” Icarus 147, 477-486.

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Dec. http://www.minorplanet.info/lightcurvedatabase.html

Zappala, V., Cellini, A., Barucci, A.M., Fulchignoni, M., Lupishko, D.E. (1990). “An analysis of the amplitude-phase relationship among asteroids.” Astron. Astrophys. 231, 548-560.

Minor Planet Bulletin 44 (2017) 331

LIGHTCURVE ANALYSIS OF HILDA ASTEROIDS In the plots below, the “Reduced Magnitude” is Johnson V as AT THE CENTER FOR SOLAR SYSTEM STUDIES: indicated in the Y-axis title. These are values that have been 2017 APRIL THRU JULY converted from sky magnitudes to unity distance by applying –5*log (rΔ) to the measured sky magnitudes with r and Δ being, Brian D. Warner respectively, the Sun-asteroid and Earth-asteroid distances in AU. Center for Solar System Studies – Palmer Divide Station The magnitudes were normalized to the given phase angle, e.g., 446 Sycamore Ave. alpha(6.5°), using G = 0.15, unless otherwise stated. The X-axis is Eaton, CO 80615 USA the rotational phase ranging from –0.05 to 1.05. [email protected] If the plot includes an amplitude, e.g., “Amp: 0.65”, this is the Robert D. Stephens amplitude of the Fourier model curve and not necessarily the Center for Solar System Studies adopted amplitude for the lightcurve. Landers, CA For the sake of brevity, only some of the previously reported (Received: 2017 July 10) results may be referenced in the discussions on specific asteroids. For a more complete listing, the reader is directed to the asteroid Lightcurves for ten Hilda asteroids were obtained at the lightcurve database (LCDB; Warner et al., 2009). The on-line Center for Solar System Studies (CS3) from 2017 April version at http://www.minorplanet.info/lightcurvedatabase.html thru July. allows direct queries that can be filtered a number of ways and the results saved to a text file. A set of text files of the main LCDB CCD photometric observations of ten Hilda asteroids were made tables, including the references with bibcodes, is also available for at the Center for Solar System Studies (CS3) from 2017 April thru download. Readers are strongly encouraged to obtain, when possible, the original references listed in the LCDB for their work. July. This is another in a planned series of papers on this group of asteroids, which is located between the outer main-belt and Jupiter 1748 Mauderli. Dahlgren et al. (1998) and Slyusarev et al. (2012) Trojans in a 3:2 orbital resonance with Jupiter. The goal is to both reported a period of 6.0 hours and amplitudes of 0.12 and 0.1 determine the spin rate statistics of the group and find pole and mag, respectively. Analysis of the CS3 data does not seem to shape models when possible. We also we look to examine the support that result. The period spectrum shows a clear minimum at degree of influence that the YORP effect (Rubincam, 2000) has on about 5.55 h, with only a very slight local minimum at 6 h. The distant objects and to compare the spin rate distribution against the CS3 lightcurve has an amplitude of 0.25 mag, which gives us Jupiter Trojans, which can provide evidence that the Hildas are confidence in the shorter period, as does forcing the CS3 data to a more “comet-like” than main-belt asteroids. period near 6 h. Even at 0.25 mag, a bimodal lightcurve is not Table I lists the telescopes and CCD cameras that are combined to certain (Harris et al., 2014); therefore, we are not overly concerned about the trimodal solution, especially given its asymmetry. make observations. Up to nine telescopes can be used for the campaign, although seven is more common. All the cameras use CCD chips from the KAF blue-enhanced family and so have essentially the same response. The pixel scales ranged from 1.24- 1.60 arcsec/pixel. All lightcurve observations were unfiltered since a clear filter can result in a 0.1-0.3 magnitude loss. The exposures varied depending on the asteroid’s brightness and sky motion.

Telescopes Cameras 0.30-m f/6.3 Schmidt-Cass FLI Microline 1001E 0.35-m f/9.1 Schmidt-Cass FLI Proline 1001E 0.35-m f/11 Schmidt-Cass SBIG STL-1001E 0.40-m f/10 Schmidt-Cass 0.50-m f/8.1 Ritchey-Chrétien Table I. List of available telescopes and CCD cameras at CS3. The exact combination for each telescope/camera pair can vary due to maintenance or specific needs.

Measurements were made using MPO Canopus. The Comp Star Selector utility in MPO Canopus found up to five comparison stars of near solar-color for differential photometry. Catalog magnitudes were usually taken from the CMC-15 (http://svo2.cab.inta-csic.es/vocats/cmc15/) or APASS (Henden et al., 2009) catalogs. The MPOSC3 catalog was used as a last resort. The last catalog is based on the 2MASS catalog (http://www.ipac.caltech.edu/2mass) with magnitudes converted from J-K to BVRI (Warner, 2007). The nightly zero points for the catalogs are generally consistent to about ±0.05 mag or better, but on occasion reach 0.1 mag and more. There is a systematic offset among the catalogs so, whenever possible, the same catalog is used throughout the observations for a given asteroid. Period analysis is also done with MPO Canopus, which implements the FALC algorithm developed by Harris (Harris et al., 1989).

Minor Planet Bulletin 44 (2017) 332

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 1748 Mauderli 04/29-05/02 125 11.2,11.4 159 2 5.552 0.003 0.25 0.02 2959 Scholl 04/18-04/30 154 15.6 133 2 4.359 0.002 0.14 0.02 3254 Bus 05/01-05/12 112 12.1,12.6 154 4 8.99 0.01 0.46 0.03 3290 Azabu 04/16-04/18 190 7.0,7.6 185 3 7.670 0.005 0.23 0.02 7174 Semois 04/29-05/03 74 12.5,12.9 159 2 7.456 0.006 0.38 0.03 8130 Seeberg 04/04-04/20 329 5.8,2.4 211 7 35.1 0.2 0.42 0.03 8130 Seeberg 05/19-06/03 397 9.1,12.5 211 7 38.10 0.03 0.23 0.03 9829 Murillo 04/06-04/22 473 1.8,6.8 191 1 21.754 0.006 0.81 0.02 13504 1988 RV12 04/29-05/20 522 5.4,4.0,4.5 232 14 26.562 0.005 0.50 0.05 15540 2000 CF18 04/13-04/24 600 5.7,7.5 197 17 28.41 0.02 0.51 0.03 22058 2000 AA64 04/22-04/30 207 6.8,8.7 191 9 17.04 0.05 0.23 0.03

Table II. Observing circumstances. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is then the second of three values. LPAB and BPAB are each the average phase angle bisector longitude and latitude (see Harris et al., 1984).

2959 Scholl. Dahlgren et al. (1998) found a period P > 16 h and amplitude A > 0.1 mag, but that result is rated U = 1 (likely wrong) in the asteroid lightcurve database (LCDB; Warner et al., 2009). Our data led to a period of 4.359 ± 0.002 h and amplitude of 0.14 mag. The low amplitude and unequal spacing of maximums vs. minimums casts a small shadow of doubt on the solution, but our data could not be fit to a longer period.

3254 Bus. Binzel and Sauter (1992) first reported a period 6.62 h with amplitude of 0.31 mag. The original analysis made only slight adjustments of nightly zero points and found a period of 8.99 h. By taking more than usual liberties with zero point adjustments, especially the one on May 1, it was possible to get a 3290 Azabu. Dahlgren et al. (1998) found P > 12 h and A > 0.08 good fit to a solution near the one from Bus and Sauter (1992). We mag for this 20 km Hilda, which is rated U = 1 in the LCDB. Our have adopted the shorter period of 6.54 h for this paper. Both analysis led what we consider a secure period of 7.670 ± 0.005 h, lightcurves are shown for comparison. Minor Planet Bulletin 44 (2017) 333

7174 Semois. The estimated diameter of this Hilda is 27 km. This appears to be the first reported result. Despite the sparse data set, the amplitude and a very good fit to a half-period of 3.73 h makes the solution reasonably secure.

9829 Murillo. Slyusarev et al. (2012) reported a period of P > 4 h. No lightcurve was published, making direct comparison of results impossible. Our result of 21.754 ± 0.006 h does tally with theirs in that the period is longer than 4 hours. Given the more than double coverage of the lightcurve and amplitude, we consider this solution to be secure. 8130 Seeberg. Warner worked Seeberg in 2017 April and found a period of about 85 h with the possibility of tumbling. When Stephens observed it a month later, there were no obvious signs of tumbling and he found a good bimodal fit to a period of 38.1 h. In light of this, the April data were revisited to see if the data would fit a period near 38 h. The period spectrum shows a sharp minimum at 35 hours, which is close but still significantly off the longer period. Maybe more data at a future apparition will lead to a stronger solution.

(13504) 1988 RV12. Stephens (2016) observed 1988 RV12 in 2016 March and reported a period of 26.543 h with an amplitude of 0.61 mag. Analysis of the data obtained by Warner in 2017 led to a similar result of 26.562 ± 0.006 h but a smaller amplitude of 0.48 mag. The 2017 observations were at a phase angle bisector longitude 60° greater than in 2016 (172° vs. 232°). It would be a

reasonable guess to say that the spin axis pole longitude is near 260° (or 80°) and the latitude |β| > 45°.

Minor Planet Bulletin 44 (2017) 334 Acknowledgements

Funding for observations, analysis, and publication for Warner and Stephens was provided by NASA grant NNX13AP56G. Work on the asteroid lightcurve database (LCDB) by Warner was also funded in part by National Science Foundation grant AST- 1507535. The authors gratefully acknowledge Shoemaker NEO Grants from the Planetary Society (2007, 2013, 2015). These were used to purchase some of the telescopes and CCD cameras used in this research. This research was made possible through the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund and in was based in on data from CMC15 Data Access Service at CAB (INTA-CSIC) (http://svo2.cab.inta-csic.es/vocats/cmc15/). This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the

Infrared Processing and Analysis Center/California Institute of (15540) 2000 CF18. This appears to be the first reported period Technology, funded by the National Aeronautics and Space for the 20-km Hilda. We consider the period secure. Administration and the National Science Foundation. (http://www.ipac.caltech.edu/2mass/)

References

Binzel, R. P., Sauter, L. M. (1992). “Trojan, Hilda, and Cybele asteroids – New lightcurve observations and analysis.” Icarus 95, 222-230.

Dahlgren, M., Lahulla, J.F., Lagerkvist, C.-I., Lagerros, J., Mottola, S., Erikson, A., Bonano-Beurer, M., Di Martino, M. (1998). “A Study of Hilda Asteroids. V. Lightcurves of 47 Hilda Asteroids.” Icarus 133, 247-285.

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, (22058) 2000 AA64. This also appears to be the first reported H., Zeigler, K.W. (1989). “Photoelectric Observations of period for 2000 AA64. The large error bars compared to the Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. amplitude of the lightcurve make the solution probable but not certain. Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, T.C., Welch, D.L. (2009). http://www.aavso.org/apass

Slyusarev, I.G., Shevchenko, V.G., Belskaya, I.N., Krugly, Yu.N., Chiorny, V.G. (2012). “CCD Photometry of Hilda Asteroids.” ACM 2012 (Niigata, Japan), #6398.

Stephens, R.D. (2016). “Asteroids Observed from CS3: 2016 January-March.” Minor Planet Bull. 43, 252-255.

Warner, B.D. (2007). “Initial Results of a Dedicated H-G Program.” Minor Planet Bul. 34, 113-119.

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Updated 2017 April. http://www.minorplanet.info/lightcurvedatabase.html

Minor Planet Bulletin 44 (2017) 335

NEAR-EARTH ASTEROID LIGHTCURVE ANALYSIS For the sake of brevity, only some of the previously reported AT CS3-PALMER DIVIDE STATION: results may be referenced in the discussions on a specific asteroid. 2017 APRIL THRU JUNE For a more complete listing, the reader is directed to the asteroid lightcurve database (LCDB; Warner et al., 2009). The on-line Brian D. Warner version at http://www.minorplanet.info/lightcurvedatabase.html Center for Solar System Studies / MoreData! allows direct queries that can be filtered a number of ways and the 446 Sycamore Ave. results saved to a text file. A set of text files of the main LCDB Eaton, CO 80615 USA tables, including the references with bibcodes, is also available for [email protected] download. When possible, readers are strongly encouraged to check against the original references listed in the LCDB. (Received: 2017 July 11) If the plot includes an amplitude, e.g., “Amp: 0.65”, this is the Lightcurves for 31 near-Earth asteroids (NEAs) obtained amplitude of the Fourier model curve and not necessarily the at the Center for Solar System Studies-Palmer Divide adopted amplitude for the lightcurve. The value is provided as a Station (CS3-PDS) from 2017 April thru June were matter of convenience. analyzed for rotation period and signs of satellites or tumbling. 1917 Cuyo. There are many previous results in the LCDB, all near 2.7 h. The 2017 data did not lead to a unique result. CCD photometric observations of 31 near-Earth asteroids (NEAs) were made at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2017 April thru June. Table I lists the telescope/CCD camera combinations used for the observations. All the cameras use CCD chips from the KAF blue-enhanced family and so have essentially the same response. The pixel scales for the combinations range from 1.24-1.60 arcsec/pixel.

Desig Telescope Camera Squirt 0.30-m f/6.3 Schmidt-Cass ML-1001E Borealis 0.35-m f/9.1 Schmidt-Cass FLI-1001E Eclipticalis 0.35-m f/9.1 Schmidt-Cass STL-1001E Australius 0.35-m f/9.1 Schmidt-Cass STL-1001E Zephyr 0.50-m f/8.1 R-C FLI-1001E Table I. List of CS3-PDS telescope/CCD camera combinations.

All lightcurve observations were unfiltered since a clear filter can result in a 0.1-0.3 magnitude loss. The exposure duration varied depending on the asteroid’s brightness and sky motion. Guiding on a field star sometimes resulted in a trailed image for the asteroid. If necessary, an elliptical aperture with the long axis parallel to the asteroid’s path was used.

Measurements were made using MPO Canopus. The Comp Star Selector utility in MPO Canopus found up to five comparison stars of near solar-color for differential photometry. Catalog magnitudes were usually taken from the CMC-15 (http://svo2.cab.inta-csic.es/vocats/cmc15/) or APASS (Henden et al., 2009) catalogs. The MPOSC3 catalog was used as a last resort. This catalog is based on the 2MASS catalog (http://www.ipac.caltech.edu/2mass) with magnitudes converted from J-K to BVRI (Warner, 2007). The nightly zero points for the catalogs are generally consistent to about ± 0.05 mag or better, but on occasion reach 0.1 mag and more. There is a systematic offset among the catalogs so, whenever possible, the same catalog is used throughout the observations for a given asteroid. Period analysis is also done with MPO Canopus, which implements the FALC algorithm developed by Harris (Harris et al., 1989).

In the plots below, the “Reduced Magnitude” is Johnson V as indicated in the Y-axis title. These are values that have been converted from sky magnitudes to unity distances by applying –5*log (rΔ) to the measured sky magnitudes with r and Δ being, respectively, the Sun-asteroid and Earth-asteroid distances in AU. The magnitudes were normalized to the given phase angle, e.g., alpha(6.5°), using G = 0.15, unless otherwise stated. The X-axis is the rotational phase, ranging from –0.05 to +1.05. Minor Planet Bulletin 44 (2017) 336

The period spectrum and half-period search both strongly favor a period of 2.911 h over one of 2.743 h. As shown in the two lightcurves, either period apparently gives the same quality fit. It’s worth noting that the two differ by exactly one-half rotation over 24 hours. Finding such aliased periods such as these can often be attributed to mismatching to which half of a symmetrical lightcurve a given data set applies. However, both of these are sufficiently asymmetrical to almost rule out that possibility.

The data from 2014 (Warner, 2014b; 2015a) were re-examined to see if they might help resolve the ambiguity. The data from May could also be equally fit to two periods of about 2.7 and 2.9 hours. However, the April data showed a decided preference for 2.7 h and an almost certain exclusion of 2.9 h. For this reason, the period of 2.743 h found from the 2017 data is the one adopted for this paper. 1980 Tezcatlipoca. This NEA always has a fairly large amplitude (0.55-1.01 mag; LCDB). The period found from the 2017 data is in excellent agreement with past results.

2329 Orthos. Warner (2017b) reported a period of 6.178 h based on data obtained in 2017 February-March. That solution appears to be wrong. Based on the period spectrum and a search of half- periods using the May data, a period of 4.6473 h was found and is adopted as the correct result. The earlier data were re-analyzed, usually by slight modifications to nightly zero points, to see if they would fit the shorter period. As the revised period spectrum shows, a period of 4.610 h is favored. However, the measurement 5653 Camarillo. The incomplete coverage of the lightcurve from error bars are significant in relation to the amplitude, which makes the data set obtained in 2017 April-May leads to a period spectrum the revised solution suspect, even if it is in near agreement with with many nearly-equal solutions. The period of 4.867 h was one based on the high-quality data set from May. adopted because it produced somewhat symmetric bimodal fit and it agreed with numerous results in the LCDB.

Minor Planet Bulletin 44 (2017) 337

5879 Almeria. No previous results were found in the LCDB for (68348) 2001 LO7. This asteroid proved to be an exception to the this 1-km NEA. rule that having an amplitude of about 0.3 mag or greater strongly favors a bimodal solution. The better (but not definitive) cutoff is about 0.38 mag (Harris et al., 2014).

(7888) 1993 UC. The solution was forced to match one found earlier (Warner, 2017a). As a stand-alone result, it is unreliable.

(11398) 1998 YP11. Pravec et al. (2005) found a period of 38.6 h. Given the period and estimated size, this asteroid is a very good candidate for non-principal axis rotation (“tumbling”). However, neither Pravec et al. or Warner (2008) found obvious signs of tumbling. This was true again based on two data sets in 2017, one in February (Warner, 2017b) and the one reported here that led to a period of 38.464 h, in good agreement with all previous results.

Minor Planet Bulletin 44 (2017) 338

Earlier results from Skiff (2011; 3.324 h) and Warner (2015b; 3.8759 h) both showed a bimodal lightcurve. Because of the larger (141056) 2001 XV4. The period spectrum for the 1.1 km asteroid amplitude in 2017, it was thought that a bimodal solution was shows numerous possibilities. most likely, which led to a solution of 1.9100 h. This places the asteroid just above the so-called “spin barrier,” which separates rubble pile asteroids (gravitationally-bound) from those that are strength-bound. However, that barrier is not hard-fast and so there was room for this asteroid to be an exception.

It took about two weeks to obtain sufficient data to break the period ambiguity by examining the “split-halves” plot. This is where the data are phased to a given period but the second half of the lightcurve is superimposed on top of the first half. If the two halves show sufficient disagreement (a subjective analysis), the period is more likely correct than the potential half-period. This plot and analysis were used to solve a similar case: 5404 Uemura (Harris et al., 2104).

Given the earlier results and the split-halves analysis, the conclusion is that the period of 3.8201 h found from the 2017 data is most likely correct.

(100926) 1998 MQ. Warner (2011) found a period of 2.328 h based on data obtained in 2010 October. The 2017 data led to the same result, although it does produce an asymmetrical lightcurve. The period spectrum showed weaker “side-lobes” (periods that differ by one-half cycle over 24 hours). Forcing the data to those produced unsatisfactory results.

(106589) 2000 WN107. This appears to be the first reported period for 2000 WN107, which has an estimated diameter of 1.9 km. The low amplitude and somewhat noisy data make the solution probable but far from certain.

Minor Planet Bulletin 44 (2017) 339

It favored a period of 2.83 hours. However, when doing a half- period search, one that doubles to about 2.67 h is favored. This is another case where the two periods differ by one-half a rotation over 24 hours. The solution of 2.671 h is adopted for this paper, based primarily on its Fourier curve having a better fit to the data.

(143404) 2003 BD44. By rights, 2003 BD44 should be in a tumbling state (Pravec et al., 2014; 2005). There are small signs of this, i.e., the data from the second and following cycles did not quite overlap those from the first cycle. However, this could also be due to changes in the lightcurve over the range of observations. If tumbling, it is at a low-level and would be nearly impossible to characterize accurately.

(163696) 2003 EB50. Using data from 2013 (Warner, 2014a), a period of 27.2 h was found, with the possibility of tumbling. Observations in 2015 (Warner, 2016a), found a period of 62.4 h (222073) 1999 HY1. Despite the noisy data, a reasonably secure with no obvious signs of tumbling. The data obtained in 2017 led solution was found. Given the amplitude, a bimodal lightcurve to a period of 62.9 h. Here again, if tumbling is present, it’s at a would not be a certainty, but the asymmetry of the lightcurve very low level and likely not to be fully characterized. moved the solution to the fore.

(215588) 2003 HF2. The data from the initial run for this 400- meter asteroid resembled what is often seen for superfast rotation, i.e., P < 1 h, with maybe a slight upward trend. A search from 0.001-1.500 h using 0.001 h steps found no hints of a very short period. This was not a surprise: the size of the asteroid made it highly unlikely for a period much less than about 2 hours. After four nights of observations and almost no adjustments to nightly zero points, it appeared that there was no long term trend and the asteroid was just too near the observing limits at the time to get a sufficient signal-to-noise ratio.

Minor Planet Bulletin 44 (2017) 340

(388838) 2008 EZ5. This NEA was first observed in 2017 March- (418094) 2007 WV4. There were no previous entries in the LCDB April. Assuming a bimodal lightcurve, a period of 2.858 h was for this 400-meter NEA. Fortunately, the amplitude was large, found. This was confirmed by a denser data set obtained a month which helped overcome the noisy data and virtually assured a later, which produced a period spectrum with fewer and more bimodal lightcurve. certain potential solutions.

(427643) 2003 VF1. This also appears to be the first reported lightcurve for this 1-km asteroid. The period is too short for the given size to expect tumbling, nor was there any evidence of such.

(441987) 2010 NY65. The unusual shape of the lightcurve was a concern, but the period of 4.973 h is in close agreement with earlier results (Warner, 2016b).

(474179) 1999 VS6. The period and size (D ~ 490 m) make this a very good candidate for tumbling (Pravec et al., 2014; 2005). With Minor Planet Bulletin 44 (2017) 341 the incomplete lightcurve and the noisy data, it would nearly impossible to detect tumbling, unless it were very pronounced.

(484795) 2009 DE47 was observed by the author in 2017 March (Warner, 2017b) at a phase angle of about 41°. It was observed again a month later, at phase angle 12°. Oddly, the amplitude was (474231) 2001 HZ7. The adopted period is a best guess. The data smaller at the larger phase angle. The anomaly may be due to the are very noisy. However, there seems to be a sufficient trend in the orientation of the spin axis and the line-of-sight to the asteroid data near 0.10 rotation phase to overcome that and so try to fit the each time. data to a low order Fourier solution. The H-G calculator in MPO Canopus was used to find the absolute magnitude (H) and phase slope parameter (G). Ideally, data below 7° phase angle would have been obtained in order to fully characterize the result for G. However, the minimum phase angle during the apparition was about 9°. The result of H = 18.76 ± 0.06 closely resembles the value in the MPCORB file (18.6). The value for G is consistent with but not confirmation of a medium albedo, e.g., pV ~ 0.2 for S-type asteroids, the type assumed for 2009 DE47.

(475665) 2006 VY13. This 1.1-km NEA was first observed in 2017 April. Despite incomplete coverage of the lightcurve, the period of 17.507 h seemed reasonably secure. This was confirmed about a month later with a denser data set and period of 17.544 h. Note how the amplitude of the lightcurve decreased from April to June, as expected with a decreasing solar phase angle (Zappala et al., 1990).

Minor Planet Bulletin 44 (2017) 342

2005 GL9, 2011 ED78, 2014 KF91. There were no previous entries in the LCDB for these three NEAs. The estimated diameters are, respectively, 1.4 km, 0.65 km, and 0.45 km.

2017 MC1. The observations for the 40-meter asteroid were made in support of radar observations using a speckle technique (Michael Busch, private communications). His main concern was that the asteroid was not spinning extremely fast.

2017 CS. The period spectrum shows numerous solutions, including those near a monomodal, bimodal, and trimodal lightcurve. None of these can be formally excluded given the amplitude of 0.05 mag. Since there was no compelling evidence to support otherwise, a bimodal lightcurve was assumed, leading to a period of 3.000 h.

Minor Planet Bulletin 44 (2017) 343

A fit to a very short period (0.001-1.500 h) was tried after the first Acknowledgements night, but there was no good solution. The second night showed similar data but were nearly 0.7 mag brighter after correcting for Funding for PDS observations, analysis, and publication was changing viewing aspect. On the assumption that the two nights provided by NASA grant NNX13AP56G. Work on the asteroid represented a minimum and immediately following maximum, lightcurve database (LCDB) was also funded in part by National several half-period and full-period solutions were tried with a 2nd Science Foundation grant AST-1507535. This research was made order Fourier fit. The aim was to find a model curve that had possible in part based on data from CMC15 Data Access Service reasonable slopes and the two extremes separated by 0.25 rotation at CAB (INTA-CSIC) (http://svo2.cab.inta-csic.es/vocats/cmc15/) phase. The end result was a solution of 33 ± 5 h for a bimodal and through the use of the AAVSO Photometric All-Sky Survey curve. This must be considered as only as a guess. (APASS), funded by the Robert Martin Ayers Sciences Fund. This publication makes use of data products from the Two Micron All 2017 JA2, 2017 GM4, 2017 FH101. There were no previous Sky Survey, which is a joint project of the University of entries in the LCDB for these NEAs. The estimated diameters are, Massachusetts and the Infrared Processing and Analysis respectively, 33 m, 120 m, and 95 m. The solutions for 2017 JA2 Center/California Institute of Technology, funded by the National and 2017 FH101 are considered secure. The one for 2017 GM4 is Aeronautics and Space Administration and the National Science less so, but still very likely correct. Foundation. (http://www.ipac.caltech.edu/2mass/)

References

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.

Harris, A.W., Pravec, P., Galad, A., Skiff, B.A., Warner, B.D., Vilagi, J., Gajdos, S., Carbognani, A., Hornoch, K., Kusnirak, P., Cooney, W.R., Gross, J., Terrell, D., Higgins, D., Bowell, E., Koehn, B.W. (2014). “On the maximum amplitude of harmonics on an asteroid lightcurve.” Icarus 235, 55-59. Henden, A.A., Terrell, D., Levine, S.E., Templeton, M., Smith, T.C., Welch, D.L. (2009). http://www.aavso.org/apass

Pravec, P., Harris, A.W., Scheirich, P., Kušnirák, P., Šarounová, L., Hergenrother, C.W., Mottola, S., Hicks, M.D., Masi, G., Krugly, Yu.N., Shevchenko, V.G., Nolan, M.C., Howell, E.S., Kaasalainen, M., Galád, A., Brown, P., Degraff, D.R., Lambert, J. V., Cooney, W.R., Foglia, S. (2005). “Tumbling asteroids.” Icarus 173, 108-131.

Pravec, P., Scheirich, P., Durech, J., Pollock, J., Kusnirak, P., Hornoch, K., Galad, A., Vokrouhlicky, D., Harris, A.W., Jehin, E., Manfroid, J., Opitom, C., Gillon, M., Colas, F., Oey, J., Vrastil, J., Reichart, D., Ivarsen, K., Haislip, J., LaCluyze, A. (2014). “The tumbling state of (99942) Apophis.” Icarus 233, 48-60.

Pravec, P., Hergenrother, C., Whiteley, R., Sarounova, L., Kusnirak, P. (2000). “Fast Rotating Asteroids 1999 TY2, 1999 SF10, and 1998 WB2.” Icarus 147, 477-486.

Skiff, B.A. (2011) Posting on CALL web site. http://www.minorplanet.info/call.html

Warner, B.D. (2007). “Initial Results of a Dedicated H-G Program.” Minor Planet Bull. 34, 113-119.

Warner, B.D. (2008). “Asteroid Lightcurve Analysis at the Palmer Divide Observatory: February-May 2008.” Minor Planet Bull. 35, 163-167.

Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Dec. http://www.minorplanet.info/lightcurvedatabase.html Minor Planet Bulletin 44 (2017) 344

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 1917 Cuyo 04/23-05/05 187 13.8,11.7 240 23 A2.743 0.001 0.16 0.02 1980 Tezcatlipoca 06/27-07/02 382 27.0,30.4 244 9 7.2492 0.0006 0.81 0.02 2329 Orthos 02/25-03/03 73 18.6,17.1 195 10 4.610 0.002 0.39 0.04 2329 Orthos 05/11-05/22 280 30.9,37.1 192 23 4.6473 0.0007 0.18 0.01 5653 Camarillo 04/29-05/12 73 48.2,46.5 159 1 4.867 0.002 0.6 0.03 5879 Almeria 06/20-06/23 109 23.3,23.2 261 30 13.67 0.05 0.45 0.05 7888 1993 UC 05/20-05/23 81 21.2,20.5 258 35 2.320 0.002 0.22 0.03 11398 1998 YP11 05/26-06/12 696 71.4,63.3 229 46 38.464 0.008 0.46 0.03 68348 2001 LO7 06/20-07/03 257 8.3,13.5 256 14 A3.8201 0.0003 0.3 0.04 100926 1998 MQ 05/23-05/27 130 10.7,12.3 241 15 2.328 0.002 0.12 0.02 106589 2000 WN107 06/03-06/19 131 36.9,26.5 296 20 3.101 0.002 0.07 0.01 141056 2001 XV4 05/23-05/29 99 52.5,48.7 292 9 A2.671 0.002 0.21 0.02 143404 2003 BD44 02/25-04/12 1818 18.1,3.3,54.4 177 1 78.863 0.003 1.05 0.05 163696 2003 EB50 05/25-06/02 295 30.5,35.1 210 18 62.9 0.2 1.42 0.05 215588 2003 HF2 04/10-04/13 281 38.5,37.2 176 1 - - <0.1 - 222073 1999 HY1 05/01-05/04 420 11.5,14.6 223 11 10.37 0.03 0.16 0.03 388838 2008 EZ5 03/27-04/03 82 18.2,17.8,18.2 202 1 2.858 0.002 0.13 0.02 388838 2008 EZ5 04/03-04/13 191 11.9,21.8 188 -1 2.859 0.002 0.13 0.02 418094 2007 WV4 06/13-06/18 296 64.5,60.5 250 38 9.929 0.005 0.65 0.05 427643 2003 VF1 04/16-04/22 369 47.0,37.4 233 28 11.470 0.003 0.7 0.03 441987 2010 NY65 06/27-06/29 593 71.2,58.3 257 29 4.973 0.003 0.24 0.02 474179 1999 VS6 04/23-04/30 316 63.5,58.6 178 16 16.91 0.05 0.51 0.04 474231 2001 HZ7 04/18-04/21 402 43.0,40.4 185 14 65. 2. 0.35 0.06 475665 2006 VY13 04/04-04/11 216 34.4,28.9 224 10 17.507 0.005 1.39 0.03 475665 2006 VY13 05/28-06/03 240 12.3,14.8 235 8 17.544 0.008 0.89 0.02 484795 2009 DE47 04/19-04/21 249 11.1,13.1 201 3 5.987 0.004 0.41 0.02 2005 GL9 05/15-05/22 237 16.5,15.0 248 12 5.131 0.001 0.24 0.02 2011 ED78 05/21-05/23 137 31.5,32.6 219 19 4.976 0.004 0.34 0.03 2014 KF91 06/03-06/19 269 18.2,28.0 245 8 18.954 0.003 0.8 0.03 2017 CS 05/24-05/27 665 82.0,76.4 204 8 3.000 0.002 0.05 0.01 2017 MC1 06/27-06/28 167 20.6,17.1 267 2 33. 5. 0.7 0.1 2017 JA2 05/11-05/11 675 54.1,54.1 205 9 3.88 0.03 0.91 0.05 2017 GM4 04/14-04/14 265 26.5,26.5 189 -2 2.878 0.002 0.45 0.05 2017 FH101 04/22-04/22 428 46.2,46.2 203 24 0.3468 0.0001 0.58 0.03 Table II. Observing circumstances. APeriod is preferred of two or more solutions. Pts is the number of data points used in the analysis. The phase angle (α) is given at the start and end of each date range, unless it reached a minimum, which is then the second of three values. LPAB and BPAB are, respectively the average phase angle bisector longitude and latitude, unless two values are given (first/last date in range). Grp is the orbital group of the asteroid. See Warner et al. (LCDB; 2009; Icarus 202, 134-146.). Warner, B.D. (2011). “Asteroid Lightcurve Analysis at the Palmer Warner, B.D. (2017a). “Near-Earth Asteroid Lightcurve Analysis Divide Observatory: 2010 September-December.” Minor Planet at CS3-Palmer Divide Station: 2016 July-September.” Minor Bull. 38, 82-86. Planet Bull. 44, 22-36.

Warner, B.D. (2014a). “Near-Earth Asteroid Lightcurve Analysis Warner, B.D. (2017b). “Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2013 September-December.” at CS3-Palmer Divide Station: 2016 December thru 2017 April.” Minor Planet Bull. 41, 113-124. Minor Planet Bull. 44, 223-237.

Warner, Brian D. (2014b). “Near-Earth Asteroid Lightcurve Zappala, V., Cellini, A., Barucci, A.M., Fulchignoni, M., Analysis at CS3-Palmer Divide Station: 2014 March-June” Minor Lupishko, D.E. (1990). “An analysis of the amplitude-phase Planet Bull. 41, 213-224. relationship among asteroids.” Astron. Astrophys. 231, 548-560.

Warner, B.D. (2015a). “Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2014 June-October.” Minor Planet Bull. 42, 41-53.

Warner, B.D. (2015b). “A Quartet of Near-Earth Asteroid Binary Candidates.” Minor Planet Bull. 42, 79-83.

Warner, B.D. (2016a). “Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2016 January-April.” Minor Planet Bull. 43, 240-250.

Warner, B.D. (2016b). “Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2016 April-July.” Minor Planet Bull. 43, 311-319.

Minor Planet Bulletin 44 (2017) 345

ASTEROIDS OBSERVED We obtained a synodic period of 6.977 ± 0.002 h with an FROM ESTCORN OBSERVATORY amplitude of 0.08 mag.

Daniel A. Klinglesmith III, Sebastian Hendrickx, Cameron Kimber Etscorn Campus Observatory New Mexico Tech 101 East Road Socorro, NM 87801, USA [email protected]

(Received: 2017 July 12 Revised: 2017 July 16)

We provide lightcurves for seven asteroids from the Spin/Shape Modeling Opportunities listed by Warner et al. (2017)

The asteroids for which we report results were selected from the list of shape/spin modeling (SSMO) opportunities given by Warner et al. (2017). We selected photometry opportunities based 901 Brunsia is a main-belt asteroid discovered by M. Wolf at on asteroid brightness and period. We wanted to be able to obtain Heidelberg on 1918 Aug 30. It is also known as 1918 EE, 1941 a complete lightcurve in one night. MH, 1948 VJ, 1970 EP1, and A905 VD. We observed in on three Our observations were obtained with three Celestron 0.35-m nights between 2017 May 20-28. We obtained a synodic period of telescopes and SBIG CCD cameras at Etscorn Campus 3.136 ± 0.001 h with an amplitude of 0.28 mag. Observatory (Klinglesmith and Franco, 2016). The images were processed and calibrated using MPO Canopus 10.4.7.6 (Warner,2015). Depending on the brightness of the asteroids, the exposures were between 180 and 420 seconds through clear filters. The multi-night data sets for each asteroid were combined with the FALC algorithm (Harris et al., 1989) within MPO Canopus to provide synodic periods for each asteroid.

Discovery information was obtained from the JPL small bodies node (JPL, 2017). The seven asteroids were suggested as possible targets in order to derive their spin / shape models (Warner et al. 2017). Table I contains the observation circumstances and results. Table II is a compilation of the previously obtained lightcurves with their references for all asteroids except for 1016 Anitra. The information for it is listed in Table III.

459 Signe is a main-belt asteroid discovered by M. Wolf at Heidelberg on 1900 Oct 22. It is also known as 1900 FM, 1934 939 Isberga is a main-belt asteroid discovered by K. Reinmuth at VH, 1938 SE1, A917 TF, and A921 RD. We observed it on five Heidelberg on 1920 Oct 4. It is also known as 1920 HR, 1930 QP, nights between 2017 Apr 23 and May 5. We obtained a synodic 1957 QE, and 1957 UU. We observed it on three nights between period of 5.538 ± 0.002 h with an amplitude of 0.28 mag. 2017 May 20-28. We obtained a synodic period of 2.917 ± 0.001 h with an amplitude of 0.21 mag.

611 Valeria is a main-belt asteroid discovered by J. H. Metcalf at

Taunton on 1906 Sep 24. It is also known as 1906 VL, and A901VA. We observed it on six nights between 2017 May 1-20. 1016 Anitra is a main-belt asteroid discovered by K. Reinmuth at Heidelberg on 1924 Jan 31. It is also known as 1924 QG and 1929 Minor Planet Bulletin 44 (2017) 346

TE1. Pilcher et al. (2016) reported that 1016 Anitra is an DS, 1965 SF, 1965 VH, 1970 EM, 1973 CE, 1975 UH, and 1975 asynchronous binary asteroid. Our observations confirm that the VE. We observed it on seven nights between Apr 14-22. We object does have two periods. We observed it on five nights obtained a synodic period of 2.834 ± 0.001 h with an amplitude of between 2017 Apr 23 and May 5. Using the single-period mode 0.24 mag. we found a synodic period of 5.930 ± 0.001 h with an amplitude of 0.28 mag. and a fair amount of scatter. Using the dual-period search within Canopus (Warner, 2015), we confirm the two periods found by Pilcher et al. Our results were P1= 5.9259 ± 0.0005 h with an amplitude of 0.26 mag and P2= 2.6090 ± 0.0002 h with an amplitude of 0.10 mag. The scatter in magnitudes was much smaller using the dual-period search. The previous results for 1016 Anitra can be found in Table III.

6009 Yuzuruyoshii is a main-belt asteroid discovered by E.F. Helin at Palomar on 1990 Mar 24. It is also known as 1990 FQ1, 1952 HE3, and 1957 WJ1. We observed it on three nights: 2017 Jun 16-18. We obtained a synodic period of 3.003 ± 0.006 h with an amplitude of 0.09 mag.

Acknowledgements

The Etscorn Campus Observatory operations are supported by the Research and Economic Development Office of New Mexico Institute of Mining and Technology (NMIMT).

References

Alkema, M.S. (2013). “Asteroid Lightcurve Analysis at Elephant Head Observatory: 2012 November - 2013 April.” Minor Planet Bull. 40, 133-137.

Behrend, R. (2001, 2002, 2003, 2005, 2006, 2007, 2011, 2015). http://obswww.unige.ch/~behrend/page_cou.html

Carry, B., Matter, A., Scheirich, P., Pravec, P., Molnar, L., Mottola, S., Carbognani, A., Jehin, E., Marciniak, A., Binzel, R.P., and 22 coauthors (2015). “The Small Binary Asteroid (939) 1967 Menzelis a main-belt asteroid discovered by M. Wolf at Isberga.” Icarus 248, 516-525. Heidelberg on 1095 Nov 1. It is also known as A905 VC, 1930

Minor Planet Bulletin 44 (2017) 347

Clark, M. (2015).“Asteroid Photometry from the Preston Gott Molnar, L.A., Haegert, M.J., Beaumont, C.N., Block, M.J., Cook, Observatory.” Minor Planet Bull. 42, 15-20. P.L., Green, A.G., Holtrop, J.P., Hoogeboom, K.M., Kulisek, J.J., Lovelace, J.S., Olivero, J.S., Shrestha, A., Taylor, J.F., and 3 Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). colleagues (2008). “Lightcurve Analysis of a Magnitude Limited “Lightcurves and phase relations of the asteroids 82 Alkmene and Asteroid Sample.” Minor Planet Bull. 35, 9-12. 444 Gyptis.” Icarus 57, 251-258. Pilcher, F. (2012). “Rotation Period Determinations for 47 Aglaja, Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., 252 Clementina, 611 Valeria, 627 Charis, and 756 Lilliana.” Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, Minor Planet Bull. 39, 220-222. H., Zeigler, K. (1989).“Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186. Pilcher, F., Benishek, V., Jacobsen, J., Kristensen, L.H., Lang, K., Larson, F.R., Odden, C., Pravec, P. (2016). “Minor Planet 1016 Higgins, D. (2008). “Asteroid Lightcurve Analysis at Hunters Hill Anitra: A Likely Asynchronous Binary.” Minor Planet Bull. 43, Observatory and Collaborating Stations: April 2007 - June 2007.” 274-277. Minor Planet Bull. 35, 30-32. Pravec, P., Wolf, M., Sarounova, L. (2006, 2007, 2010). JPL Small Body Database Search Engine. (2017). http://www.asu.cas.cz/~ppravec/neo.htm http://ssd.jpl.nasa.gov/sbdb_query.cgi Pray, D.P. (2006). “Lightcurve Analysis of Asteroids 326, 329, Klinglesmith III, D.A., Franco, L. (2016). “Lightcurves for 1531 619, 1967, 2453, 10518 and 42267.” Minor Planet Bull. 33, 4-5. Hartmut and 4145 Maximova.” Minor Planet Bull. 43, 121. Pray, D.P., Galad, A., Gajdos, S., Vilagi, J., Cooney, W., Gross, Klinglesmith III, D.A., Hendrickx, S., Madden, K., Montgomery, S., Terrel, D., Higgens, D., Husarik, M., Kusnirak, P. (2006). S. (2016a). “Asteroid Lightcurves from Etscorn Observatory.” “Lightcurve Analysis of Asteroids 53, 698, 1016, 1523, 1950, Minor Planet Bull. 43, 234-239. 4608, 5080, 6170, 7760, 8213, 11271, 14257, 15350 and 17509.” Minor Planet Bull. 33, 92-95. Klinglesmith III, D.A., Hendrickx, S., Madden, K., Montgomery, S. (2016b). “Lightcurves for Shape/Spin Models.” Minor Planet Schmidt, R.E. (2016). “NIR Minor Planet Photometry from Bull. 43, 123-128. Burleith Observatory, 2015.” Minor Planet Bull. 43, 129-131.

Koff, R.A. (2001). “Lightcurve photometry of 611 Valeria and Vander Haagen, G.A. (2009). “Lightcurves and H-G parameters 986 Amelia.” Minor Planet Bull. 28, 77-78. for 901 Brunsia and 946 Poesia.” Minor Planet Bull. 36, 136-138.

Kryszczynska, A., Colas, F., Polinska, M., Hirsch, R., Ivanova, V., Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid Apostolovska, G., Bilkina, B., Velichko, F.P., Kwiatkowski, T., Lightcurve Database.” Icarus 202, 134-146. Updated 2016 Sep. Kankiewicz, P., and 20 coauthors. (2012). “Do Slivan states exist http://www.minorplanet.info/lightcurvedatabase.html in the Flora family?. I. Photometric survey of the Flora region.” Astron. Astrophys. 546, A72. Warner, B.D. (2015). MPO Canopus software. http://www.minorplanetobserver.com/MPOSoftware/ Lagerkvist, C.-I., Rickman, H. (1982). “Physical studies of MPOCanopus.htm asteroids. IX - The light curve of the M asteroid 77 Frigga.” Moon &Planets 27, 107-110. Warner, B.D., Harris, A.W., Durech, J., Benner, L.A.M. (2017). “Lightcurve Photometry Opportunities: July-September.” Minor LeCrone, C., Duncan, A., Hudson, E., Johnson, J., Mulvihill, A., Planet Bul. 44, 161-164. Reichert, C., Ditteon, R. (2006). “2005-2006 Fall Observing Campaign at Rose-Hulman Institute of Technology.” Minor Wisniewski, W.Z., Michalowski, T.M., Harris, A.W., McMillan, Planet Bull. 33, 66-67. R.S. (1997). “Photometric Observations of 125 Asteroids.” Icarus 126, 395-449. Liu, J. (2016). “Rotation Period Analysis for 1967 Menzel.” Minor Planet Bull. 43, 98-99.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. Grp 459 Signe 04/23-05/05 207 1.4,5.9 209 0 5.538 0.002 0.28 0.03 MB-M 611 Valeria 05/01-05/20 486 3.2,7.5 220 9 6.977 0.002 0.08 0.05 MB-O 901 Brunsia 05/20-05/28 104 10.2,14.0 221 -3 3.316 0.001 0.28 0.07 MB-I 939 Isberga 05/20-05/28 85 8.8,12.7 224 -4 2.917 0.001 0.21 0.05 MB-I 1016 Anitra 04/23-05/20 244 4.1,15.6 205 -3 5.930 0.001 0.28 0.05 MB-I 1967 Menzel 04/14-04/22 318 5.7,9.3 193 3 2.834 0.001 0.24 0.03 MB-I 6007 Yuzuruyoshii 06/16-06/18 119 15.4,15.6 263 25 3.033 0.006 0.09 0.05 PHO

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009).

Minor Planet Bulletin 44 (2017) 348

Num Name References Date LPAB BPAB Phase Period Amp 459 Signe This paper 2017 Apr 29 209 0 4.1 5.538 0.28 Lagerkvist 1978 1974 Apr 20 165 9 7.2 6.38 0.25 Behrend 2007 2007 Feb 09 45 5 26.9 5.5362 0.43 611 Valeria This paper 2017 May 10 220 9 4.7 6.977 0.08 Koff 2001 2001 Mar 20 177 -4 1.7 10.8 0.09 Behrend 2002 2002 May 31 250 14 5.0 6.9814 0.16 Behrend 2003 2003 Jul 19 321 13 10.0 6.98 0.10 Behrend 2005 2005 Jan 02 55 -13 18.2 6.98 0.08 Pilcher 2012 2012 Apr 29 231 10 5.7 6.977 0.08 901 Brunsia This paper 2017 May 24 221 -3 12.2 3.136 0.28 Wisniewski 1997 1991 Oct 08 355 5 15.3 4.872 0.12 Behrend 2001 2001 Oct 02 7 6 4.5 3.1357 0.11 Vander Haagen 2009 2009 Jan 08 82 0 13.1 3.1363 0.28 Behrend 2011 2011 Oct 20 20 5 5.5 3.1335 0.17 Klinglesmith 2016a 2016 Feb 01 122 -3 4.3 3.136 0.09 939 Isberga This paper 2017 May 24 223 -4 10.8 2.917 0.21 Molnar 2008 2006 Feb 28 129 1 13.1 2.9173 0.25 Behrend 2011 2011 Nov 23 30 3 18.3 2.917067 0.22 Carry 2015 2011 Oct 26 27 3 4.8 2.91695 0.20 1967 Menzel This paper 2017 Apr 18 193 3 7.5 2.834 0.24 Pray 2006 2005 Sep 24 19 -4 12.6 2.8350 0.28 LeCrone 2006 2005 Nov 02 23 -3 11.6 2.834 0.38 Pravec 2007 2007 Apr 10 195 4 3.1 2.8344 0.24 Higgins 2008 2007 Apr 10 195 4 3.1 2.8346 0.25 Behrend 2005 2005 Oct 27 22 -3 8.2 2.83481 0.27 Pravec 2010 2010 Jan 14 151 5 18.8 2.8343 0.25 Clark 2015 2015 Jun 15 230 0 15.2 2.8364 0.39 Liu 2016 2015 Oct 11 18 -4 2.7 2.84 0.28 Klinglesmith 2016b 2015 Nov 06 20 -3 15.0 2.835 0.29 Behrend 2016 2015 Nov 05 20 -3 14.5 2.83497 0.27 6009 Yuzuruyoshii This paper 2017 Jun 17 147 26 15.5 3.033 0.09 Pravec 2006 2006 Aug 10 349 25 21.1 3.0302 0.15 Behrend 2006 2006 Sep 16 351 22 12.4 3.0304 0.14 Pravec 2010 2010 Sep 21 19 11 12.4 3.030 0.10 Table II: Summation of solar bisector angles, phase angles, periods and amplitudes for the asteroids discussed in this paper.

Num Name References Date LPAB BPAB Phase Period Amp 1016 Anitra This paper 2017 Apr 30 205 -3 7.5 5.930 0.28 Pray 2006 2005 Oct 10 10 1 4.6 5.928 0.30 Kyrszczynska 2012 2005 Sep 29 9 0 2.2 5.9288 0.28 Alkema 2013 2012 Dec 07 94 9 13.4 5.929 0.42 Schmidt 2016 2015 Oct 30 27 3 6.6 5.9301 0.27 Pilcher 2016 2015 Nov 08 27 4 11.8 5.92951 0.30 Pilcher 2016 2015 Oct 05 25 2 9.2 5.92943 0.30 Pilcher 2016 2015 Oct 15 26 2 3.5 5.9294 0.28 Pilcher 2016 2015 Nov 06 27 4 10.7 5.9295 0.28 Pilcher 2016 2015 Nov 18 29 4 17.0 5.92960 0.33 Pilcher 2016 2015 Dec 18 35 5 27.2 5.9300 0.41 Table III: Summation of solar bisector angles, phase angles, periods and amplitudes for 1016 Anitra.

Minor Planet Bulletin 44 (2017) 349

ROTATION PERIOD DETERMINATION FOR 3892 DEZSO AND 14339 KNORRE

Alessandro Marchini Astronomical Observatory, DSFTA - University of Siena (K54) Via Roma 56, 53100 - Siena, ITALY [email protected]

Riccardo Papini Carpione Observatory (K49) Spedaletto, Florence, ITALY

Fabio Salvaggio 21047 - Saronno, ITALY

(Received: 2017 July 12)

Photometric observations of two main-belt asteroids were made from the Astronomical Observatory of the University of Siena (Italy) in order to determine their synodic rotation periods. For 3892 Dezso, we found a period of 3.629 h with an amplitude of 0.47 mag. For 14339 Knorre, the period was 3.795 h with an amplitude of 0.21 mag.

CCD photometric observations of two main-belt asteroids were carried out in 2017 May at the Astronomical Observatory of the University of Siena (K54), a facility of the Department of Physical Sciences, Earth and Environment (DSFTA, 2017). We used a 0.30-m f/5.6 Maksutov-Cassegrain telescope, SBIG STL-6303E CCD camera, and clear filter. The pixel scale was 2.30 arcsec with binning of 2x2 pixels. All exposures were 300 sec. Data processing and analysis were done with MPO Canopus (BDW 14339 Knorre (1983 GU) was discovered on1983 April 10 by L. I. Publishing, 2017). All the images were calibrated with dark and Chernykh at the Crimean Astrophysical Observatory and is named flat-field frames and converted to R magnitudes using solar- in honor of Ernest Khristov Knorre (1759-1810) who was the first colored field stars from a version of the CMC-15 catalogue astronomer at Tartu University. The asteroid orbits with a semi- distributed with MPO Canopus. Table I shows the observing major axis of about 2.601 AU, eccentricity 0.174, inclination circumstances and results. 14.40°; the orbital period is 4.19 years. Its absolute magnitude is H = 12.4 (JPL, 2017; MPC, 2017). A search of the asteroid lightcurve database (LCDB; Warner et al., 2009) indicates that our results may be the first reported lightcurve observations and results for these objects.

3892 Dezso (1941 HD) was discovered on 1941 April 19 by L. Oterma at Turku and is named in honor of the Hungarian astronomer Dezso Lorant, founder of the Observatory for Solar Physics in Debrecen and its director for many years. The asteroid orbits with a semi-major axis of about 2.605 AU, eccentricity 0.141, inclination 13.76°; the orbital period is 4.20 years. According to MPC (2017), JPL (2017), and WISE (Masiero et al., 2012), the absolute magnitude is H = 12.5 and D = 7.836 ± 0.907 km. This leads to an optical albedo of pV = 0.315 ± 0.063.

A total of 159 data points were obtained over four nights. The period analysis shows a clear bimodal solution at P = 3.629 ± 0.001 h with an amplitude A = 0.47 ± 0.02 mag.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E Amp A.E. Grp 3892 Dezso 05/24-28 159 11.3,10.9 249.3 19.1 3.629 0.001 0.47 0.02 EUN 14339 Knorre 05/15-18 125 13.6,12.6 254.5 14.5 3.795 0.002 0.21 0.03 EUN

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given at the start and end of each date range, unless it reached a minimum, which is the second of three values. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984). Grp is the asteroid family/group (Warner et al., 2009; Zappalà et al., 1997).

Minor Planet Bulletin 44 (2017) 350

STULL OBSERVATORY LIGHTCURVE OBSERVATIONS: 1998-2002

David R DeGraff Physics & Astronomy Alfred University 1 Saxon Dr Alfred, NY 14802 [email protected]

(Received: 2017 July 15)

Using the Stull Observatory 0.82m telescope, from July 1998 to August 2002 we observed several asteroids to measure their rotation periods. We present lightcurves periods for 314 Rosalia, 1084 Tamarwina, 1758 Naantali, 1845 Helewalda, 2544 Gubarev, 3028 Zhangguoxi, 5215 Tsurui, (20713) 1999 XA32, and Observations of this asteroid were conducted on three nights, (234871) 1991 GT4. collecting a total of 125 data points. The period analysis shows a bimodal solution with P = 3.795 ± 0.002 h with an amplitude Between 1998 July and 2002 August, we used the Stull A = 0.21 ± 0.03 mag. Observatory 0.82-m f/4 Newtonian telescope to observe asteroid lightcurves. Our first observations used an SBIG-ST6 CCD Acknowledgements camera with a Bessel R filter. After 1999 May we were able to hit The authors want to thank Piero Giannini, a high school student much fainter targets with a Finger Lakes Instruments camera with from Istituto “Tito Sarrocchi” (Siena) involved in an interesting a rear-illuminated TK 1024 chip. We took biases and dark current vocational guidance project about astronomy, for his help during frames every night, and twilight flats fields when possible. The the data reduction of some observing sessions. flats had very little variation in them from one night to the next, so missing a few nights of flats was not a problem. References We chose our targets among the asteroids near opposition in the DSFTA (2017), Dipartimento di Scienze Fisiche, della Terra e 14 to 16 magnitude range: the faintest we can get good signal-to- dell'Ambiente – Astronomical Observatory. noise ratios with 90 to 120-second integrations. When there was a http://www.dsfta.unisi.it/en/department/science- choice of targets, we chose members of dynamical families. museums/astronomical-observatory We observed each asteroid in the R filter until it got close to the Harris, A.W., Young, J.W., Scaltriti, F., Zappalà, V. (1984). meridian, then we would observe in V and R and take exposures in “Lightcurves and phase relations of the asteroids 82 Alkmene and V and R of nearby secondary standard stars from the LONEOS 444 Gyptis.” Icarus 57, 251-258. catalog (Skiff). Unfortunately, the skies downwind from the Great Lakes are not very stable, so the values given for the individual JPL (2017). Small-Body Database Browser. asteroids are only accurate to about 0.1 magnitudes. This is not http://ssd.jpl.nasa.gov/sbdb.cgi#top very reliable, so all magnitudes reported should be taken as instrumental values instead of being on any standard scale. Masiero, J.R., Mainzer, A.K., Grav, T., Bauer, J.M., Cutri, R.M., Nugent, C., Cabrera, M.S. (2012). “Preliminary Analysis of We analyzed our images using the CCDPHOT aperture WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic photometry package in IDL (Buie, 2000) choosing the aperture Observations of Main Belt Asteroids.” Astrophys. J. 759, L8. with the highest S/N. We then used Dahlgren’s technique (Dahlgren et al., 1991) to perform the ensemble photometry with MPC (2017). MPC Database. five to twelve reference stars. We corrected the times for light http://www.minorplanetcenter.net/db_search/ delay and adjusted the magnitudes for earth and sun distances of 1.0 AU. Warner, B.D. (2017). MPO Software, MPO Canopus v10.7.7.0. Bdw Publishing. http://minorplanetobserver.com We then used an IDL program using Harris’s Fourier fitting technique (Harris et al., 1989) to find the period. This method Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid takes a range of periods, calculates the phase, does a four- Lightcurve Database.” Icarus 202, 134-146. Updated 2017 April. component Fourier fit, and then plots the values of χ2 as a function http://www.minorplanet.info/lightcurvedatabase.html of period. The various minimum values in the χ2 plot can be explored to look for physically reasonable fits. Once a period has Zappalà, V., Bendjoya, P., Cellino, A., Farinella, P., Froeschle, C. been determined, we can find the night-to-night offset (produced (1997). “Asteroid Dynamical Families. EAR-A-5-DDR-FAMILY- by changing distance from the Earth and Sun as well as viewing V4.1.” NASA Planetary Data System geometry and inaccuracies in the ability to place our observations on the standard magnitude scale) then find the optimum number of terms used in the Fourier fit, and re-calculate the best period from the Fourier scan. We iterated through this process until it converged on a solution.

Minor Planet Bulletin 44 (2017) 351

We tested the reliability of our period-determining code by 1758 Naantali is a member of the Eos family with H = 10.9 (SBN, measuring previously known rotation periods, using results 2017). We found a highly symmetric double-peaked lightcurve obtained in MPO Canopus v10.4.7.6 in observations from 2007 with a period of 5.47 ± 0.03 h. This is consistent with other results (Stoelting) and finding rotation periods published after we made from Behrend (2010), Waszczak (2016), and Durech (2016). our observations. This last test is a symptom of severe Hollow squares are 2000 May 3 and solid squares are 2000 procrastination and is not recommended. May 4. The phase zero-point is JD 2451182.5 (LTC)

314 Rosalia is an SMASS class C asteroid with an absolute 1758 Naantali Period = 5.47 ± 0.03 h magnitude H = 9.5 ± 0.15, a diameter of 59.7 ± 2.2 km, and an albedo of 0.0787 ± 0.006 (SBN, 2017). We measured its period to be 16.8 ± 0.2 hours. Our results are almost consistent with Behrend’s (2004) period of 15.84 ± 0.05 h but not with the 20.4 h period obtained by Hawkins (2008) and Warner (2006). The closest χ2 minimum to that period was 19.8 h, but there are gaps in the curve which have unrealistic amplitudes in the fit. Open squares are 2002 Jun 18, solid squares are 2002 Jun 20 and open triangles are 2002 Jun 21. The zero-point for the phase is JD 2452443.5 (LTC).

314 Rosalia Period = 16.8 ± 0.2 h

1845 Helewalda is an Eros family member with H = 11.3 (SBN, 2017). We found the lightcurve best represented by a 7.35 ± 0.13 h, which is consistent with results from Carbo (2009), Brinsfield (2010), Behrend (2010), and Waszczak (2016) who all got periods around 7.4 hours. Open squares from 2001 Jun 18, filled squares from the 2001 Jun 19, and open triangles from 2001 Jun 20. The zero-point for the phase is JD 2450778.5 (LTC).

1845 Helwalda Period = 7.35 ± 0.13 h

1084 Tamarwina is a C class asteroid with an absolute magnitude H = 10.78, an albedo of 0.1165 ± 0.018 and a diameter of 27.2 ± 1.9 km (SBN, 2017). The lightcurve for this asteroid shows a period of 6.153 ± 0.001 h. The previously published 7.08 hour period (Binzel 1987), which had less than full phase coverage, is within 15% of our full phase coverage period. The asteroid has also been measured by Ivarson (2004), Behrend (2007), Sada (2008), and Stecher (2008), all of whom found periods around 6.2 hours (LCDB; Warner et al., 2009). Open squares are for 1998 Jul 16, solid squares are for 1998 Jul 19, open triangles are for 1998 Jul 21, solid triangles are for 1998 Jul 27, and open diamonds are for 1998 Jul 28. The phase zero-point is JD 2451010.5 (LTC).

1084 Tamariwa Period = 6.153±0.001 h

2544 Gubarev a member of the Phocaea family, has an absolute magnitude H = 12.3, diameter of 9.4 ± 0.4 km, and albedo of 0.243 ± 0.025 (SBN, 2017). The rotation period of 4.8 hours is very close to one-fifth of a day, so the three nights together didn’t pin the period down any better than we got in a single night. Each of the individual nights gave us a period of 4.8 ± 0.2 hours. Nominally, the best period for the combined data, using a four- component Fourier fit is 4.7519 ± 0.0018 hours, but 4.66 h and 4.84 h were almost as good a fit because of the ambiguity of the number of rotations from one day to the next. Bolt (2007), Pravec (2012), and Behrend (2012) also obtained periods of 4.75 hours. Open squares are from 2002 Aug 4, filled squares are from 2002 Aug 14, and triangles are from 2002 Aug 19. The zero-point for the phase is JD 2452500.5 (LTC). Minor Planet Bulletin 44 (2017) 352

Number Name yyyy/ mm/dd-mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 314 Rosalia 2002/06/18-06/21 94 6.1,6.0 268 15 16.9 0.2 0.26 0.05 1084 Tamariwa 1998/07/16-07/28 68 4.0,2.8,4.2 299 5 6.153 0.001 0.27 0.05 1758 Naantali 2000/05/03-05/04 28 5.4 223 13 5.47 0.03 0.46 0.05 1845 Helewalda 2001/06/18-06/20 105 5.3,5.7 217 6 7.35 0.13 0.34 0.05 2544 Gubarev 2002/08/04-08/19 181 6.5,4.35,5.1 322 8 4.7519 0.0018 0.45 0.05 3028 Zhangguoxi 2002/05/16-06/03 111 7,13 217 6 4.383 0.003 0.24 0.05 5215 Tsurui 2001/06/01-06/19 129 9.7,7.7,8.2 261 14 2.08 0.01 0.18 0.05 20713 1999 XA32 2002/08/01 41 5.6 321 7 3.5 0.2 0.23 0.05 23481 1991 GT4 2002/08/03-08/19 116 8.6,4.6,5.4 321 6 5.958 0.007 0.65 0.05 Table I. Observing circumstances and results. Pts is the number of data points. The phase angle values are for the first and last date, unless

a minimum (second value) was reached. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

results include Behrend (2009; 3.76 h), Hamanowa (2011; 3.836 ± 0.002 h, and Stephens (2005; 3.81 h). Our observations show a peak in the χ2 plot at 3.7 hours instead of a minimum, so those results are not consistent with ours. Filled squares are from 2000 Jun 1 and the open squares are from 2000 Jun19. The zero-point for the phase is JD 2450779.5 (LTC).

5215 Tsurui Period = 2.08 ± 0.01 h

3028 Zhangguoxi is a member of the Eos family with a Bus class of K; it has an absolute magnitude H = 10.7, diameter of 25.6 ± 1.4 km, and albedo 0.142 ± 0.017 (SBN, 2017). Using a 3- component Fourier fit, we found a period of 4.383 ± 0.003 hours, consistent with the 4.4 h period of Gross (2011), but slightly off from the 4.8 h periods found by Behrend (2007), Brinsfield (2007), and Stephens (2007). Filled squares are from 2002 May16, (20713) 1999 XA32 serendipitously drifted through the field while open squares are from 2002 May 23, open triangles are from 2002 we were observing 23481 on 2002 Aug 1. This asteroid has an June 1, filled triangles are from 2002 Jun 2, and open diamonds absolute magnitude of 11.7. We were able to find a two- are from 2002 Jun 3. The phase zero-point is JD 2452410.5 component Fourier fit that has a rotational period of 3.5 ± 0.2 h. (LTC). Waszczak (2016) found a period of 3.548 ± 0.005 h. The zero- point for the phase is JD 2452487.5 (LTC). 3028 Zhangguoxi Period = 4.383 ± 0.003 h (20713) 1999 XA32 Period = 3.5 ± 0.2 h

(234871) 1991 GT4, a possible member of the Baptistina or Flora 5215 Tsurui. The absolute magnitude of Tsurui, a member of the families, has an absolute magnitude of H = 14.3, and an SDSS Eunomia family, is H = 11.2 (SBN, 2017). We found a period with 2 taxonomy class of S (SBN, 2017). We found a period of 5.958 ± a well-defined dip in the χ function at 2.08 ± 0.01 hours. Other 0.007 h, although a slightly less better period of 5.81 hours is also Minor Planet Bulletin 44 (2017) 353 possible. The open squares are from 2002 Aug 3, the filled squares Dahlgren, M., Fitzsimmons, A., Lagerkvist, C.I., Williams, I.P. 2002 Aug 14, and the open triangles 2002 Aug 19. There did not (1991). “Differential CCD photometry of Dubiago, Chiron, and seem to be any other published periods for this asteroid when we Hektor.” MNRAS 250, 115. checked the Small Body Node on 2017 Jun 19 or on the LCDB (Warner 2009). The phase zero-point is JD = 2452489.5 (LTC). Durech, J., Hanus, J., Oszkiewsicz, D., Vanco, R. (2016). “Asteroid models from the Lowell photometric database.” Astron. (23481) 1991 GT4 Period = 5.948 ± 0.007 Astrophys. 587, A48.

Gross, J. (2011). Posting on CALL site. http://www.minorplanet. info/ call.html

Hamanowa, H., Hamanowa, H. (2011). http://www2.ocn.ne.jp/ ~hamaten/astlcdata.htm

Harris, A.W., Young, J.W., Scaltriti, F., Zappala, V. (1984). “Lightcurves and phase relations of the asteroids 82 Alkmene and 444 Gyptis.” Icarus 57, 251-258.

Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne, H., Zeigler, K.W. (1989). “Photoelectric Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.

Hawkins, S., Ditteon, R. (2008). “Asteroid Lightcurve Analysis at the Oakley Observatory - May 2007.” Minor Planet Bull. 35, 1-4. Acknowledgements Sada, P.V. (2008). “Lightcurve Analysis of 1084 Tamariwa.” I wish to acknowledge the contributions of the various summer Minor Planet Bull. 35, 50. research students over the years who were instrumental in helping obtain and analyze the data: Adrienne Robbins, Ryan Boas, Rob SBN (2017). NASA Planetary Data System: Small Bodies Node, Gutermuth, Jessie Crast, Joy Lambert, Jamie Kern, and Carolyn last visited on 2017 Jun 19. https://pds-smallbodies.astro. umd.edu/ Windus. We would also like to thank Marc Buie of SWRI Observatory for making his IDL routines available, and Brian Skiff, B. (1999). LONEOS Star Catalog (last access 2002 Aug Skiff, also of Lowell, for his list of secondary standard stars. This 18). ftp://ftp.lowell.edu/pub/bas/starcats/loneos.phot research has also made use of the Small Bodies Data Ferret (http://sbn.psi.edu/ferret/), supported by the NASA Planetary Stecher, G., Ford, L., Lorenzen, K., Ulrich, S. (2008). System. “Photometric Measurements of 1084 Tamariwa at Hobbs Observatory.” Minor Planet Bull. 35, 76-77. References Stephens, R.D. (2005). “Asteroid lightcurve photometry from Behrend, R. (2004, 2007, 2009, 2010, 2012). Observatoire de Santana Observatory - Spring 2005.” Minor Planet Bull. 32, 82- Geneve web site. 83. http://obswww.unige.ch/~behrend/ page_cou.html Stephens, R.D. (2007). “Photometry from GMARS and Santana Binzel, R.P. (1987). “A photoelectric survey of 130 asteroids.” Observatories - April to June 2007.” Minor Planet Bull. 34, 102- Icarus 72, 135-208. 103. Bolt, G., Bembrick, C. (2007). “Lightcurve Analysis of Minor Stoelting, M., DeGraff D.R. (2016). “Lightcurve Results For Planets 2544 Gubarev and 2599 Veseli.” Minor Planet Bull. 34, Asteroids 900 Rosalinde, 4666 Dietz, and 6302 Tengukogen.” 43. Minor Planet Bull. 43, 44-45. Brinsfield, J.W. (2007). “The Rotation Periods of 873 Holda, 3028 Pravec, P., Wolf, M., Sarounova, L. (2012). Zhangguoxi 3497 Innanen, 5484 Inoda, 5654 Terni, and 7304 http://www.asu.cas.cz/ ~ppravec/neo.htm Namiki.” Minor Planet Bul. 34, 108-110. Warner, B.D. (2006). “Asteroid lightcurve analysis at the Palmer Brinsfield, J.W. (2010). “Asteroid Lightcurve Analysis at the Via Divide Observatory - March - June 2006.” Minor Planet Bull. 33, Capote Observatory: 2010 February-May.” Minor Planet Bul. 37, 85-88. 146-147. Warner, B.D., Harris, A.W., Pravec, P. (2009). “The asteroid Buie, Marc (2001). An Introduction to CCDPHOT (May 20) lightcurve database.” Icarus 202, 134-146. Updated 2016 July 19. http://www.boulder.swri.edu/~buie/idl/ccdphot.html http://www.MinorPlanet.info/ lightcurvedatabase.html Carbo, L., Green, D., Kragh, K., Krotz, J., Meiers, A., Patino, B., Pligge, Z., Shaffer, N., Ditteon, R. (2009). “Asteroid Lightcurve Analysis at the Oakley Southern Sky Observatory: 2008 October thru 2009 March.” Minor Planet Bull. 36, 152-157.

Minor Planet Bulletin 44 (2017) 354

Waszczak, A., Chang, C.-K., Ofek, E.O., Laher, R., Masci, F., Levitan, D., Surace, J., Cheng, Y.-C., Ip, W.-H., Kinoshita, D., Helou, G., Prince, T.A., Kulkarni, S. (2015). “Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry.” Astron. J. 150, A75.

ROTATION PERIOD DETERMINATION FOR 3760 POUTANEN AND 14309 DEFOY

Fabio Salvaggio Gruppo Astrofili Catanesi 21047 – Saronno, ITALY [email protected]

Alessandro Marchini Astronomical Observatory, DSFTA - University of Siena (K54) Via Roma, 56, 53100 – Siena, ITALY

Riccardo Papini Carpione Observatory (K49) San Casciano in Val di Pesa (FI), ITALY

(Received: 2017 July 14 Revised: 2017 July 21)

Photometric observations of the main-belt asteroids 3760 Poutanen and 14309 Defoy were performed in 2017 April-May. The data revealed a tri-modal lightcurve phased to a period of 2.956 ± 0.001 hours for 3760 Poutanen and a bimodal lightcurve phased to 3.391 ± 0.002 hours for 14309 Defoy. 14309 Defoy (A908 SA, 1992 SU1) was discovered on 1908 September 22 by J. Palisa at Vienna. Its orbit has a semi-major Lightcurve analysis we report here was performed using images taken at the Astronomical Observatory of the University of Siena axis of 2.605 AU, eccentricity 0.447, and period of 4.21 years (Italy). The equipment consisted of a 0.30-m f/5.6 Maksutov- (JPL, 2017). We observed Defoy on 2017 May 21-24. The Cassegrain telescope, SBIG STL-6303E NABG CCD camera, and collaborative observations resulted in 3 sessions with a total of clear filter; the pixel scale was 2.30 arcsec with 2x2 binning. 124 data points. We found a bimodal lightcurve with a synodic period of 3.391 ± 0.002 h and amplitude of 0.16 ± 0.02 mag. Exposures were 300 seconds. The images were calibrated with dark and flat-field frames. MPO Canopus (Warner, 2017) was used to measure the images, do Fourier analysis, and produce the lightcurves. Table I lists the observation circumstances and results.

3760 Poutanen (1984 AQ) was discovered on 1984 January 8 by E. Bowell at Flagstaff. Its orbit has a semi-major axis of 2.532 AU, eccentricity 0.184, and period of 4.03 years (JPL, 2017). We observed this asteroid from 2017 April 23-30. The collaborative observations resulted in 3 sessions with a total of 172 data points. Our analysis found a tri-modal lightcurve phased to 2.956 ± 0.001 h with an amplitude of 0.19 ± 0.03 mag.

Number Name 2017 mm/dd Pts Phase LPAB BPAB Period(h) P.E. Amp A.E. 3760 Poutanen 04/23-30 172 13.8,11.2 231.5 13.7 2.956 0.001 0.19 0.03 14309 Defoy 05/21-24 124 8.7,8.2 245.5 10.0 3.391 0.002 0.16 0.02

Table I. Observing circumstances and results. Pts is the number of data points. The phase angle is given for the first and last date. LPAB and BPAB are the approximate phase angle bisector longitude and latitude at mid-date range (see Harris et al., 1984).

Minor Planet Bulletin 44 (2017) 355

LIGHTCURVE PHOTOMETRY OPPORTUNITIES: 2017 OCTOBER-DECEMBER

Brian D. Warner Center for Solar System Studies / MoreData! 446 Sycamore Ave. Eaton, CO 80615 USA [email protected]

Alan W. Harris MoreData! La Cañada, CA 91011-3364 USA

Josef Ďurech Astronomical Institute Charles University 18000 Prague, CZECH REPUBLIC [email protected] References Lance A.M. Benner Harris, A.W., Young, J.W., Scaltriti, F., Zappalà, V. (1984). Jet Propulsion Laboratory “Lightcurves and phase relations of the asteroids 82 Alkmene and Pasadena, CA 91109-8099 USA 444 Gyptis.” Icarus 57, 251-258. [email protected]

JPL (2017). Small-Body Database Browser. We present lists of asteroid photometry opportunities for http://ssd.jpl.nasa.gov/sbdb.cgi#top objects reaching a favorable apparition and have no or poorly-defined lightcurve parameters. Additional data Warner, B.D., Harris, A.W., Pravec, P. (2009). “The Asteroid on these objects will help with shape and spin axis Lightcurve Database.” Icarus 202, 134-146. Updated 2017 April. modeling via lightcurve inversion. We also include lists http://www.minorplanet.info/lightcurvedatabase.html of objects that will be the target of radar observations. Lightcurves for these objects can help constrain pole Warner, B.D. (2017). MPO Software, MPO Canopus v10.7.7.0. solutions and/or remove rotation period ambiguities that Bdw Publishing. http://minorplanetobserver.com might not come from using radar data alone.

We present several lists of asteroids that are prime targets for photometry during the period 2017 October-December.

In the first three sets of tables, “Dec” is the declination and “U” is the quality code of the lightcurve. See the asteroid lightcurve data base (LCDB; Warner et al., 2009) documentation for an explanation of the U code:

http://www.minorplanet.info/lightcurvedatabase.html

The ephemeris generator on the CALL web site allows you to create custom lists for objects reaching V ≤ 18.5 during any month in the current year, e.g., limiting the results by magnitude and declination.

http://www.minorplanet.info/PHP/call_OppLCDBQuery.php

We refer you to past articles, e.g., Minor Planet Bulletin 36, 188, for more detailed discussions about the individual lists and points of advice regarding observations for objects in each list.

Once you’ve obtained and analyzed your data, it’s important to publish your results. Papers appearing in the Minor Planet Bulletin are indexed in the Astrophysical Data System (ADS) and so can be referenced by others in subsequent papers. It’s also important to make the data available at least on a personal website or upon request. We urge you to consider submitting your raw data to the ALCDEF page on the Minor Planet Center web site:

http://www.minorplanetcenter.net/light_curve

Minor Planet Bulletin 44 (2017) 356

We believe this to be the largest publicly available database of raw Low Phase Angle Opportunities lightcurve data that contains 2.5 million observations for more than 11500 objects. The Low Phase Angle list includes asteroids that reach very low phase angles. The “α” column is the minimum solar phase angle Now that many backyard astronomers and small colleges have for the asteroid. Getting accurate, calibrated measurements access to larger telescopes, we have expanded the photometry (usually V band) at or very near the day of opposition can provide opportunities and spin axis lists to include asteroids reaching important information for those studying the “opposition effect.” V = 15.3 and brighter. Use the on-line query form for the LCDB

Lightcurve/Photometry Opportunities http://www.minorplanet.info/PHP/call_OppLCDBQuery.php

Objects with U = 3– or 3 are excluded from this list since they will to get more details about a specific asteroid. likely appear in the list below for shape and spin axis modeling. Those asteroids rated U = 1 should be given higher priority over You will have the best chance of success working objects with low those rated U = 2 or 2+, but not necessarily over those with no amplitude and periods that allow covering at least half a cycle period. On the other hand, do not overlook asteroids with U = 2/2+ every night. Objects with large amplitudes and/or long periods are on the assumption that the period is sufficiently established. much more difficult for phase angle studies since, for proper Regardless, do not let the existing period influence your analysis analysis, the data must be reduced to the average magnitude of the since even high quality ratings have been proven wrong at times. asteroid for each night. This reduction requires that you determine Note that the lightcurve amplitude in the tables could be more or the period and the amplitude of the lightcurve; for long period less than what’s given. Use the listing only as a guide. objects that can be difficult. Refer to Harris et al. (1989; Icarus 81, 365-374) for the details of the analysis procedure. An entry in bold italics is a near-Earth asteroid (NEA). As an aside, some use the maximum light to find the phase slope Brightest LCDB Data parameter (G). However, this can produce a significantly different Number Name Date Mag Dec Period Amp U ------value for both H and G versus when using average light, which is 5964 1990 QN4 10 01.1 14.9 +2 the method used for values listed by the Minor Planet Center. 5189 1990 UQ 10 01.5 14.2 -58 1182 Ilona 10 01.9 13.5 +13 29.8 0.98- 1.2 2 1422 Stromgrenia 10 03.9 14.6 +5 3.5 0.24-0.29 2 The International Astronomical Union (IAU) has adopted a new 763 Cupido 10 04.1 14.0 +12 14.88 0.03 1 system, H-G12, introduced by Muinonen et al. (2010; Icarus 209, 1134 Kepler 10 06.0 14.3 +15 9513 1971 UN 10 07.1 15.0 +0 542-555). However it will be some years before it becomes the 25980 2001 FK53 10 07.3 14.8 +2 general standard and, furthermore, it is still in need of refinement. 916 America 10 09.0 12.9 +24 38. 0.28 1 3744 Horn-d'Arturo 10 11.0 14.6 +10 7.093 0.28-0.45 2 That can be done mostly through having more data for more 5561 Iguchi 10 11.2 14.8 +19 112.4 0.43 2 asteroids, but only if there are data at very low and moderate phase 1283 Komsomolia 10 12.3 13.6 -2 96. 1.03 1+ angles. Therefore, we strongly encourage observers to obtain data 2967 Vladisvyat 10 12.9 14.7 +1 10357 1993 SL3 10 13.0 14.8 +12 2.762 0.05 2- for these objects not only at very low phase angles, but to follow 16009 1999 CM8 10 16.8 14.1 +1 16.7 0.54-0.65 2+ them well before and/or after opposition, i.e., out to phase angles 4576 Yanotoyohiko 10 17.4 15.0 +0 16852 Nuredduna 10 18.9 14.9 +10 of 15-30 degrees. 1287 Lorcia 10 19.4 15.0 +9 2884 Reddish 10 26.5 15.0 +12 Num Name Date α V Dec Period Amp U 2003 UV11 10 29.0 14.4 +5 ------4605 Nikitin 10 30.2 15.0 +18 846 Lipperta 01 06.5 0.16 14.0 +22 1641. 0.30 2 1953 Rupertwildt 10 30.6 14.9 +12 158 Koronis 01 14.7 0.20 12.8 +21 14.218 0.28-0.43 3 2123 Vltava 10 31.5 14.8 +16 34. 0.19-0.21 2 212 Medea 01 25.7 0.30 12.2 +20 10.283 0.03-0.16 3 2597 Arthur 11 04.0 15.0 +14 54 Alexandra 01 30.8 0.25 12.0 +18 7.024 0.10-0.31 3 21766 1999 RW208 11 04.5 14.8 +18 177 Irma 02 04.0 0.40 13.2 +17 13.856 0.24-0.37 3 2908 Shimoyama 11 04.7 15.0 +20 103 Hera 02 10.3 0.28 11.5 +15 23.740 0.35-0.45 3 8484 1988 VM2 11 04.8 14.7 +10 2.548 0.15 2 924 Toni 02 13.8 0.39 13.7 +12 19.437 0.1 -0.24 3 1290 Albertine 11 06.5 14.8 +27 379 Huenna 03 01.4 0.16 13.9 +07 14.141 0.07-0.12 3 1711 Sandrine 11 11.6 14.8 +1 243 Ida 03 02.8 0.21 13.6 +07 4.634 0.40-0.86 3 2052 Tamriko 11 13.0 14.1 +14 7.462 0.11-0.15 2 269 Justitia 03 02.9 0.30 13.2 +08 33.128 0.14-0.25 3 5049 Sherlock 11 14.0 14.8 +18 16 Psyche 03 03.2 0.30 10.3 +08 4.196 0.03-0.42 3 666 Desdemona 11 14.8 12.4 +14 14.607 0.07-0.22 2+ 33 Polyhymnia 03 10.1 0.22 13.8 +05 18.608 0.13-0.21 3 1255 Schilowa 11 15.0 13.7 +20 29.536 0.09-0.15 2 589 Croatia 03 16.9 0.12 13.4 +01 24.821 0.16-0.25 2+ 444584 2006 UK 11 15.7 14.5 +33 356 Liguria 03 20.1 0.37 11.8 -01 31.82 0.22 3- 2430 Bruce Helin 11 17.5 13.9 +29 128. 0.60-0.61 2 77 Frigga 03 28.5 0.21 12.2 -03 9.012 0.07-0.20 3 4692 SIMBAD 11 23.1 15.0 +20 332 Siri 04 09.9 0.31 13.5 -07 8.007 0.10-0.35 3 163696 2003 EB50# 11 24.8 13.1 +27 62.4 0.73-1.43 2+ 258 Tyche 04 19.5 0.26 12.6 -11 10.041 0.09-0.43 3 1883 Rimito 11 25.4 14.2 +7 104 Klymene 05 13.9 0.22 13.2 -19 8.984 0.26-0.3 3 6484 Barthibbs 11 30.4 15.0 +9 886 Washingtonia 05 21.4 0.21 13.9 -21 9.001 0.12 3 823 Sisigambis 11 30.8 12.9 +22 146. 0.7 2 1319 Disa 05 27.2 0.36 13.4 -22 7.080 0.26-0.27 3 2638 Gadolin 12 01.9 14.4 +20 116 Sirona 05 28.2 0.17 11.2 -22 12.028 0.42-0.55 3 2790 Needham 12 03.9 14.9 +32 394 Arduina 05 29.6 0.18 12.8 -22 16.53 0.28-0.54 3 868 Lova 12 06.0 13.0 +16 41.3 0.10-0.40 2 596 Scheila 05 30.6 0.32 11.7 -21 15.848 0.06-0.10 3 1599 Giomus 12 07.5 14.6 +28 6.46 0.04-0.40 1 346 Hermentaria 06 21.9 0.13 10.8 -23 28.43 0.07-0.20 2 2971 Mohr 12 08.0 14.7 +23 691 Lehigh 06 22.2 0.31 13.4 -24 12.891 0.12-0.16 2+ 2697 Albina 12 08.2 15.0 +24 16.587 0.16-0.16 2 40 Harmonia 06 23.4 0.23 9.3 -23 8.910 0.13-0.36 3 529 Preziosa 12 09.3 13.7 +26 27. 0.56 2 767 Bondia 06 27.2 0.38 13.8 -24 4083 Jody 12 11.2 14.9 +2 539 Pamina 06 27.6 0.19 13.3 -23 13.903 0.10-0.22 3 1181 Lilith 12 11.6 13.2 +23 15.04 0.11 2 1784 Benguella 06 29.1 0.08 14.0 -23 1888 Zu Chong-Zhi 12 16.0 14.1 +20 15.9 0.28-0.50 2 10 Hygiea 06 29.8 0.21 9.1 -24 27.630 0.09-0.33 3 3881 Doumergua 12 16.7 15.0 +28 1112 Polonia 07 21.7 0.34 14.0 -21 82.5 0.20 2 2008 WM64 12 22.9 14.7 +29 382 Dodona 08 09.1 0.19 12.8 -15 4.113 0.39-0.42 3 7496 Miroslavholub 12 23.4 14.3 +22 17.87 0.14 2 271 Penthesilea 09 08.6 0.38 13.3 -05 18.787 0.33 3 3030 Vehrenberg 12 25.1 15.0 +26 4.812 0.60 2 120 Lachesis 09 10.1 0.34 12.1 -04 46.551 0.14-0.22 3 4690 Strasbourg 12 28.8 14.9 +36 69.2 0.75-0.80 2 107 Camilla 09 13.3 0.17 12.0 -03 4.844 0.32-0.53 3 2091 Sampo 12 30.0 14.2 +18 71.34 0.38 2 994 Otthild 09 26.6 0.30 12.6 +02 5.95 0.09-0.15 2+ Minor Planet Bulletin 44 (2017) 357

Num Name Date α V Dec Period Amp U Brightest LCDB Data ------Num Name Date Mag Dec Period Amp U 184 Dejopeja 10 07.1 0.32 12.9 +06 6.455 0.25-0.3 3 ------122 Gerda 10 07.4 0.22 12.3 +05 10.685 0.10-0.26 3 2228 Soyuz-Apollo 11 22.2 14.6 +17 5.3846 0.4-0.54 3- 186 Celuta 10 07.9 0.13 10.7 +06 19.842 0.4 -0.55 3 151 Abundantia 11 23.7 12.5 +24 9.864 0.15-0.20 3 658 Asteria 10 10.1 0.39 13.9 +08 21.034 0.22-0.32 3 1443 Ruppina 11 24.7 14.9 +18 5.88 0.27-0.35 3 435 Ella 10 16.9 0.11 12.1 +09 4.623 0.30-0.45 3 775 Lumiere 11 30.3 14.3 +32 6.103 0.19-0.28 3 207 Hedda 10 18.6 0.27 12.5 +09 30.098 0.09-0.11 3 608 Adolfine 11 30.8 14.7 +32 8.3458 0.16-0.37 3 24 Themis 10 19.9 0.06 11.5 +10 8.374 0.09-0.14 3 535 Montague 12 01.1 12.5 +19 10.2482 0.18-0.25 3 964 Subamara 10 25.4 0.19 14.0 +12 6.868 0.11-0.25 3 126 Velleda 12 05.1 12.1 +26 5.3672 0.07-0.22 3 673 Edda 10 29.4 0.32 13.8 +14 22.340 0.12-0.21 3 359 Georgia 12 05.4 12.5 +32 5.537 0.16-0.54 3 154 Bertha 10 30.3 0.12 12.2 +14 25.224 0.04-0.20 3 909 Ulla 12 05.9 14.0 -2 8.73 0.08-0.24 3 300 Geraldina 11 06.9 0.04 13.8 +16 6.842 0.15-0.32 3 653 Berenike 12 06.6 13.6 +8 12.4886 0.03-0.11 3 188 Menippe 11 23.2 0.12 12.9 +20 11.98 0.28 3- 326 Tamara 12 07.8 13.5 +49 14.445 0.10-0.27 3 823 Sisigambis 11 30.8 0.40 13.0 +22 146. 0.05-0.7 2 1741 Giclas 12 08.6 14.9 +24 2.943 0.10-0.15 3 1181 Lilith 12 11.7 0.21 13.3 +23 15.04 0.13 2 388 Charybdis 12 11.4 12.9 +32 9.516 0.14-0.25 3 1663 van den Bos 12 13.1 0.19 13.9 +23 740. 0.80 3- 1096 Reunerta 12 11.5 14.1 +23 13.036 0.20-0.39 3 199 Byblis 12 17.2 0.34 13.6 +22 5.220 0.05-0.15 3 217 Eudora 12 12.2 14.4 +8 25.272 0.08-0.31 3 59 Elpis 12 12.5 11.3 +9 13.69 0.07-0.42 3 295 Theresia 12 13.8 12.8 +24 10.73 0.11-0.22 3- 1072 Malva 12 16.5 13.9 +33 10.08 0.17-0.17 3 Shape/Spin Modeling Opportunities 1113 Katja 12 17.8 13.1 +41 18.465 0.08-0.17 3 980 Anacostia 12 18.9 11.4 +32 20.117 0.05-0.21 3 840 Zenobia 12 21.6 14.7 +24 5.565 0.08-0.28 3 Those doing work for modeling should contact Josef Ďurech at the 1848 Delvaux 12 22.3 15.0 +25 3.637 0.57-0.69 3 email address above. If looking to add lightcurves for objects with 1084 Tamariwa 12 22.7 14.9 +18 6.1961 0.25-0.42 3 781 Kartvelia 12 23.2 14.8 +4 19.04 0.16-0.28 3- existing models, visit the Database of Asteroid Models from 1304 Arosa 12 23.9 13.9 +26 7.7478 0.13-0.38 3 Inversion Techniques (DAMIT) web site 954 Li 12 26.4 14.8 +22 7.207 0.11-0.25 3 1116 Catriona 12 28.9 13.0 +51 8.832 0.09-0.20 3 772 Tanete 12 29.0 13.0 +48 17.258 0.07-0.18 3 http://astro.troja.mff.cuni.cz/projects/asteroids3D 114 Kassandra 12 29.1 11.4 +16 10.7431 0.23-0.25 3 8256 Shenzhou 12 29.2 14.6 +36 3.395 0.30-0.31 3 An additional dense lightcurve, along with sparse data, could lead 779 Nina 12 29.5 11.8 +26 11.186 0.06-0.32 3 to the asteroid being added to or improving one in DAMIT, thus increasing the total number of asteroids with spin axis and shape models. Radar-Optical Opportunities

Included in the list below are objects that: There are several resources to help plan observations in support of radar. 1. Are rated U = 3– or 3 in the LCDB Future radar targets: 2. Do not have reported pole in the LCDB Summary table http://echo.jpl.nasa.gov/~lance/future.radar.nea.periods.html 3. Have at least three entries in the Details table of the LCDB Past radar targets: where the lightcurve is rated U ≥ 2. http://echo.jpl.nasa.gov/~lance/radar.nea.periods.html The caveat for condition #3 is that no check was made to see if the Arecibo targets: lightcurves are from the same apparition or if the phase angle http://www.naic.edu/~pradar/sched.shtml bisector longitudes differ significantly from the upcoming http://www.naic.edu/~pradar apparition. The last check is often not possible because the LCDB does not list the approximate date of observations for all details Goldstone targets: records. Including that information is an on-going project. http://echo.jpl.nasa.gov/asteroids/goldstone_asteroid_schedule.html

Favorable apparitions are in bold text. NEAs are in italics. However, these are based on known targets at the time the list was prepared. It is very common for newly discovered objects to move Brightest LCDB Data Num Name Date Mag Dec Period Amp U up the list and become radar targets on short notice. We ------recommend that you keep up with the latest discoveries the Minor 2647 Sova 10 02.8 14.6 +11 9.366 0.23-0.35 3 Planet Center observing tools 851 Zeissia 10 03.3 14.4 +1 9.34 0.38-0.53 3 1107 Lictoria 10 04.7 14.0 -5 8.5616 0.16-0.30 3 1309 Hyperborea 10 06.2 14.4 +8 13.88 0.34-0.41 3 In particular, monitor NEAs and be flexible with your observing 658 Asteria 10 10.1 13.9 +8 21.034 0.22-0.28 3 program. In some cases, you may have only 1-3 days when the 607 Jenny 10 18.1 14.3 +23 8.521 0.17-0.26 3 224 Oceana 10 18.3 12.1 +14 9.401 0.09-0.14 3 asteroid is within reach of your equipment. Be sure to keep in 1426 Riviera 10 18.6 14.8 +20 4.4044 0.30-0.31 3 touch with the radar team (through Dr. Benner’s email listed 7505 Furusho 10 18.9 13.0 -3 4.14 0.52-0.75 3 66146 1998 TU3 10 23.8 12.0 -36 2.375 0.07-0.15 3 above) if you get data. The team may not always be observing the 159 Aemilia 10 24.8 12.3 +3 24.476 0.17-0.24 3 target but your initial results may change their plans. In all cases, 554 Peraga 10 25.6 11.2 +17 13.7128 0.11-0.28 3 1100 Arnica 10 26.3 14.5 +14 14.535 0.09-0.28 3 your efforts are greatly appreciated. 663 Gerlinde 10 28.7 14.1 +21 10.251 0.19-0.35 3 895 Helio 10 29.9 12.8 +41 9.347 0.10-0.23 3 Use the ephemerides below as a guide to your best chances for 558 Carmen 11 01.9 13.1 +3 11.387 0.2-0.31 3 111 Ate 11 03.3 11.2 +23 22.072 0.08-0.18 3 observing, but remember that photometry may be possible before 300 Geraldina 11 07.0 13.8 +16 6.8423 0.13-0.32 3 and/or after the ephemerides given below. Note that geocentric 987 Wallia 11 07.4 13.3 +30 10.0813 0.11-0.36 3 positions are given. Use these web sites to generate updated and 1028 Lydina 11 08.3 13.7 +13 11.68 0.22- 0.7 3 905 Universitas 11 09.9 12.9 +19 14.238 0.22-0.33 3 topocentric positions: 972 Cohnia 11 11.0 12.6 +28 18.472 0.19-0.21 3 420 Bertholda 11 11.1 13.0 +20 11.04 0.24-0.29 3 MPC: http://www.minorplanetcenter.net/iau/MPEph/MPEph.html 454 Mathesis 11 13.9 13.1 +21 8.378 0.20-0.37 3 2144 Marietta 11 17.6 14.8 +15 5.489 0.40-0.44 3- JPL: http://ssd.jpl.nasa.gov/?horizons 1590 Tsiolkovskaja 11 19.8 14.5 +18 6.731 0.10- 0.4 3

Minor Planet Bulletin 44 (2017) 358

In the ephemerides below, ED and SD are, respectively, the Earth Asteroid Period Amp App Last R SNR and Sun distances (AU), V is the estimated Johnson V magnitude, 3200 Phaethon 3.60 0.07 10 2016 1120 A and α is the phase angle. SE and ME are the great circles distances NEA,PHA 0.34 639 G (in degrees) of the Sun and Moon from the asteroid. MP is the (140158) 2001 SX169 - - - - 343 A lunar phase and GB is the galactic latitude. “PHA” indicates that NEA 20 G the object is a “potentially hazardous asteroid”, meaning that at (276703) 2004 BL11 - - - - 16 A some (long distant) time, its orbit might take it very close to Earth. NEA (418849) 2008 WM64 - - - - 1760 A About YORP Acceleration NEA,PHA 100 G (294739) 2008 CM 3.05 0.18 2 2015 21 A Many, if not all, of the targets in this section are near-Earth NEA 0.49 asteroids. These objects are particularly sensitive to YORP acceleration. YORP (Yarkovsky–O'Keefe–Radzievskii–Paddack) Table I. Summary of radar-optical opportunities in 2017 Oct-Dec. Data from the asteroid lightcurve database (Warner et al., 2009; is the asymmetric thermal re-radiation of sunlight that can cause Icarus 202, 134-146). If no period is given, 4 hours was assumed to an asteroid’s rotation period to increase or decrease. High calculate the radar SNR. precision lightcurves at multiple apparitions can be used to model the asteroid’s sidereal rotation period and see if it’s changing. To help focus efforts in YORP detection, Table I gives a quick summary of this quarter’s radar-optical targets. It usually takes four apparitions to have sufficient data to determine if the asteroid rotation rate is changing under the The family or group for the asteroid is given under the number influence of YORP. So, while obtaining a lightcurve at the current name. Also under the name will be additional flags such as “PHA” apparition may not result in immediately seeing a change, the data for Potentially Hazardous Asteroid or “Bin” to indicate the are still critical in reaching a final determination. This is why asteroid is a binary (or multiple) system. If followed by “?” it observing asteroids that already have well-known periods can still means that the asteroid is a suspect but not confirmed binary. The be a valuable use of telescope time. It is even more so when period is in hours and, in the case of binary, for the primary. The considering BYORP (binary-YORP) among binary asteroids Amp column gives the known range of lightcurve amplitudes. The where that effect has stabilized the spin so that acceleration of the App columns gives the number of different apparitions at which a primary body is not the same as if it would be if there were no lightcurve period was reported while the Last column gives the satellite. year for the last reported period. The “R SNR” column indicates the estimated radar SNR using the tool at Asteroid Period Amp App Last R SNR 3122 Florence 2.36 0.12 7 2016 56900 A http://www.naic.edu/~eriverav/scripts/radarscript.php NEA,PHA, Bin? 0.27 3240 G (5189) 1990 UQ - 0.78 - - 2006 A The estimate in Table I is based on using the Arecibo (A) or NEA 117 G Goldstone (G) radar. The estimate uses the current MPCORB 1989 VB 16 0.32 1 1997 79900 A absolute magnitude (H), a period of 4 hours if it’s not known, and NEA,PHA 4500 G the approximate minimum Earth distance during the three-month 2329 Orthos 4.6 - 1 2017 468 A period covered by this paper. NEA 27 G 2014 UR116 - - - - 312 A If the SNR value is in bold text, the object was found on the radar NEA 18 G planning pages listed above. Otherwise, the search tool at (171576) 1999 VF11 - 0.08 - - 8290 A NEA,PHA 471 G http://www.minorplanet.info/PHP/call_OppLCDBQuery.php (66146) 1998 TU3 2.375 0.07 5 2010 813 G NEA 0.15 46 A was used to find known NEAs that were V < 18.0 during the 2003 UV11 - - - - 4290 A quarter. An object was placed on the list only if the estimated NEA,PHA 244 G radar SNR > 10. This would produce a very marginal signal, not 1989 UP 6.98 1.16 1 1989 612 A enough for imaging, but might allow improving orbital NEA,PHA 35 G parameters. (190208) 2006 AQ 182. 0.25 1 2014 271 A NEA, Bin? 15 G 3122 Florence (Oct-Dec, H = 14.1, PHA) (162004) 1991 VE 13.48 1.08 2 2014 35 A Pravec et al. (1998) found a period of 2.358 h. Warner (2016) NEA 1.11 reported it as a suspected binary after finding a second period of (457768) 2009 KN4 - - - - 14 A 10.36 h with an amplitude of 0.07 mag. No signs of mutual events NEA were seen, however. If the second period is real, it might also be (99907) 1989 VA 2.51 0.22 2 1997 23 A due to low-level tumbling. The SNRs for the radar teams are going NEA 0.40 to be extremely large and so they are planning hi-res imaging. 3361 Orpheus 3.53 0.22 3 2013 890 A NEA 0.32 51 G DATE RA Dec ED SD V α SE ME MP GB (138852) 2000 WN10 4.46 0.38 3 2015 23 A ------10/01 17 34.4 +73 25 0.22 1.02 13.6 78.2 89 95 +0.77 +31 NEA,PHA 0.44 10/11 17 04.8 +75 21 0.29 1.04 14.1 74.4 89 85 -0.67 +33 (444584) 2006 UK - - - - 2210 A 10/21 16 48.7 +76 46 0.34 1.06 14.4 69.7 91 89 +0.02 +33 NEA 1260 G 10/31 16 44.7 +78 19 0.39 1.10 14.6 64.6 94 99 +0.79 +33 11/10 16 53.7 +80 23 0.43 1.14 14.7 59.4 99 78 -0.59 +32 (333888) 1998 ST4 - - - - 16 A 11/20 17 25.9 +83 10 0.47 1.19 14.8 54.1 103 101 +0.02 +29 NEA 11/30 19 21.8 +86 21 0.50 1.24 14.9 48.8 109 87 +0.82 +27 (163696) 2003 EB50 62. 0.73 3 2017 4160 A 12/10 00 55.0 +86 00 0.53 1.30 15.0 43.7 115 85 -0.53 +23 12/20 02 57.8 +80 55 0.56 1.36 15.1 39.0 120 114 +0.03 +19 NEA,PHA 0.83 238 G 12/30 03 41.9 +74 41 0.61 1.42 15.2 35.3 124 61 +0.86 +15 Minor Planet Bulletin 44 (2017) 359

(5189) 1990 UQ (Oct, H = 17.9) (171576) 1999 VP11 (Oct, H = 18.6, PHA) Southern Hemisphere observers get the best opportunities for this Skiff et al. (2012) were not able to find a period from data 0.8 km NEA. There is no period in the LCDB. Watch for unusual obtained in 2008. The amplitude at the time was about 0.08 mag. lightcurve shapes during the early part of the month, when the The estimated diameter is about 340 meters. phase angle is large and shadowing effects may come into play. DATE RA Dec ED SD V α SE ME MP GB DATE RA Dec ED SD V α SE ME MP GB ------10/22 17 25.0 -16 58 0.02 0.99 14.9 125.8 53 28 +0.05 +10 10/01 22 52.7 -57 33 0.07 1.03 14.3 60.1 116 47 +0.77 -53 10/23 20 34.2 -28 25 0.02 1.00 12.6 84.8 94 59 +0.10 -34 10/04 23 42.5 -45 00 0.08 1.06 14.4 47.3 129 39 +0.96 -67 10/24 22 40.1 -26 50 0.02 1.01 12.6 59.4 119 76 +0.16 -61 10/07 00 05.1 -35 50 0.10 1.08 14.7 38.9 137 51 -0.98 -77 10/25 23 34.9 -23 49 0.03 1.02 13.1 48.4 130 77 +0.24 -72 10/10 00 17.7 -29 18 0.12 1.10 15.0 33.4 143 81 -0.77 -82 10/26 00 02.4 -21 45 0.05 1.03 13.6 43.0 135 72 +0.32 -78 10/13 00 25.9 -24 31 0.15 1.12 15.3 29.9 146 116 -0.44 -84 10/27 00 18.4 -20 23 0.06 1.04 14.1 40.1 138 65 +0.41 -80 10/16 00 31.6 -20 54 0.17 1.14 15.6 27.7 148 150 -0.15 -82 10/28 00 28.9 -19 25 0.07 1.05 14.4 38.2 139 56 +0.51 -81 10/19 00 36.0 -18 02 0.19 1.17 15.9 26.5 149 158 -0.01 -80 10/29 00 36.3 -18 41 0.08 1.06 14.8 37.1 140 47 +0.61 -81 10/22 00 39.5 -15 42 0.22 1.19 16.2 25.8 149 128 +0.05 -78 10/30 00 41.8 -18 07 0.09 1.07 15.1 36.3 141 37 +0.70 -81 10/25 00 42.5 -13 45 0.25 1.21 16.5 25.6 148 95 +0.24 -76 10/31 00 46.1 -17 40 0.11 1.08 15.3 35.8 141 27 +0.79 -80 10/28 00 45.3 -12 04 0.27 1.23 16.7 25.7 147 62 +0.51 -75 (66146) 1998 TU3 (Oct-Nov, H = 14.5) 1989 VB (Oct, H = 19.8, PHA) This is one of the larger targets this quarter, the diameter being Wisniewski et al. (1997) reported a period of 16 h. The estimated about 3.7 km. The NEA has been observed at several apparitions. diameter is about 325 m, making it likely that the period is about 2 The period of about 2.37 h and low amplitudes in the past make it hours or more. Unfortunately, the NEA hovers near the galactic a good candidate for being a binary asteroid. High-precision plane for most of October. observations with dense coverage over 1-3 cycles for at least 3-4 consecutive nights will maximize the chances of finding a DATE RA Dec ED SD V α SE ME MP GB satellite. ------10/01 05 34.0 -43 08 0.02 1.00 14.2 81.0 98 106 +0.77 -32 10/03 05 50.2 -25 37 0.02 1.00 14.4 80.0 99 103 +0.91 -24 DATE RA Dec ED SD V α SE ME MP GB 10/05 05 59.2 -12 28 0.03 1.01 14.8 78.7 100 86 +0.99 -17 ------10/07 06 04.9 -03 12 0.03 1.01 15.1 77.1 101 62 -0.98 -12 10/01 03 55.9 -08 13 0.23 1.16 13.3 43.7 127 104 +0.77 -43 10/09 06 08.7 +03 23 0.04 1.01 15.4 75.3 103 36 -0.86 -8 10/06 03 47.1 -12 31 0.21 1.15 13.0 40.5 132 43 -1.00 -46 10/11 06 11.4 +08 11 0.04 1.01 15.6 73.3 104 12 -0.67 -5 10/11 03 33.1 -17 48 0.18 1.14 12.6 37.7 136 50 -0.67 -52 10/13 06 13.3 +11 48 0.05 1.01 15.9 71.2 106 25 -0.44 -3 10/16 03 11.6 -24 11 0.16 1.12 12.3 36.7 138 114 -0.15 -58 10/15 06 14.6 +14 37 0.06 1.02 16.1 69.1 108 51 -0.24 -1 10/21 02 39.5 -31 26 0.14 1.10 12.1 39.0 136 138 +0.02 -66 10/17 06 15.4 +16 51 0.06 1.02 16.2 66.8 110 77 -0.08 +0 10/26 01 53.5 -38 43 0.13 1.08 12.1 45.5 129 89 +0.32 -73 10/19 06 15.8 +18 41 0.07 1.02 16.4 64.5 112 103 -0.01 +1 10/31 00 52.9 -44 35 0.13 1.06 12.2 55.6 118 44 +0.79 -73 11/05 23 43.5 -47 40 0.13 1.04 12.6 67.4 105 79 -0.99 -66 11/10 22 37.1 -47 50 0.14 1.01 13.0 79.3 93 141 -0.59 -57 2329 Orthos (Oct-Jan, H = 14.6) 11/15 21 41.8 -46 00 0.15 0.98 13.6 90.6 80 116 -0.12 -48 The estimated diameter is 3.4 km. Warner (2017) reported a period of about 4.6 h based on observations in 2017 Feb and May. 2003 UV11 (Oct, H = 19.5, PHA) There is no reported lightcurve period for this 370 m NEA. The DATE RA Dec ED SD V α SE ME MP GB large range of phase angles makes this an excellent opportunity to ------10/10 21 11.1 -77 30 0.20 1.02 13.9 78.6 90 113 -0.77 -34 find reliable H and G parameters, i.e., absolute magnitude and 10/20 01 02.8 -64 54 0.29 1.10 14.3 60.9 105 108 +0.00 -52 phase slope parameter, respectively. 10/30 01 40.6 -54 25 0.39 1.19 14.8 50.7 111 59 +0.70 -61 11/09 01 55.3 -46 59 0.51 1.29 15.4 44.3 115 101 -0.70 -67 11/19 02 04.3 -41 00 0.63 1.38 15.9 40.0 116 117 +0.00 -70 DATE RA Dec ED SD V α SE ME MP GB 11/29 02 12.1 -35 46 0.76 1.48 16.3 37.1 115 43 +0.73 -71 ------12/09 02 20.0 -31 02 0.90 1.57 16.8 35.0 114 120 -0.64 -70 10/15 02 44.3 +12 20 0.24 1.22 17.7 17.1 159 101 -0.24 -42 12/19 02 28.7 -26 41 1.04 1.67 17.2 33.5 111 107 +0.01 -68 10/17 02 39.4 +12 11 0.21 1.20 17.3 14.9 162 129 -0.08 -43 12/29 02 38.2 -22 41 1.20 1.76 17.6 32.3 107 33 +0.77 -65 10/19 02 32.7 +11 58 0.18 1.17 16.8 12.2 166 157 -0.01 -44 01/08 02 48.6 -19 00 1.36 1.85 17.9 31.3 103 142 -0.59 -62 10/21 02 23.3 +11 39 0.15 1.14 16.3 8.8 170 175 +0.02 -45 10/23 02 09.4 +11 09 0.12 1.12 15.6 4.3 175 148 +0.10 -47 10/25 01 47.6 +10 18 0.10 1.09 14.9 2.7 177 119 +0.24 -50 2014 UR116 (Oct, H = 14.6, PHA) 10/27 01 09.8 +08 35 0.07 1.06 14.6 13.3 166 86 +0.41 -54 There is no period in the LCDB for this 350 m NEA. 10/29 23 56.3 +04 35 0.05 1.03 14.4 33.2 145 44 +0.61 -56 10/31 21 38.4 -03 52 0.04 1.01 14.9 70.0 108 21 +0.79 -39

DATE RA Dec ED SD V α SE ME MP GB ------1989 UP (Oct-Nov, H = 20.8, PHA) 10/15 07 25.4 +53 16 0.07 1.01 16.9 79.9 96 48 -0.24 +26 The estimated diameter is only 200 meters. This would make it a 10/16 06 27.2 +54 41 0.08 1.02 16.7 70.5 105 66 -0.15 +18 10/17 05 33.5 +54 23 0.08 1.03 16.6 62.0 114 84 -0.08 +11 possible candidate for being a superfast rotator, i.e,. P < 2 hours. 10/18 04 48.6 +52 57 0.09 1.05 16.5 54.6 121 102 -0.03 +5 However, Wisniewski et al. (1997) found this to have a period on 10/19 04 13.1 +50 56 0.10 1.06 16.6 48.1 128 118 -0.01 +0 the slower side of average, 6.98 h. 10/20 03 45.5 +48 44 0.11 1.07 16.6 42.6 133 132 +0.00 -5 10/21 03 24.0 +46 32 0.11 1.08 16.7 37.9 138 143 +0.02 -9 10/22 03 07.1 +44 29 0.12 1.10 16.8 33.8 142 149 +0.05 -12 DATE RA Dec ED SD V α SE ME MP GB 10/23 02 53.5 +42 36 0.13 1.11 16.9 30.3 146 148 +0.10 -15 ------10/24 02 42.5 +40 53 0.14 1.12 17.0 27.3 149 141 +0.16 -17 10/10 02 17.7 -06 04 0.14 1.13 17.7 20.1 157 45 -0.77 -61 10/14 02 35.4 -05 22 0.12 1.10 17.4 21.5 156 95 -0.33 -57 10/18 02 59.3 -04 09 0.10 1.08 17.0 23.6 154 140 -0.03 -52 10/22 03 32.3 -02 09 0.08 1.07 16.7 27.3 151 164 +0.05 -44 10/26 04 18.8 +01 00 0.07 1.05 16.4 33.7 144 139 +0.32 -33 10/30 05 22.5 +05 27 0.06 1.03 16.4 44.1 134 109 +0.70 -17 11/03 06 40.3 +10 25 0.05 1.02 16.6 57.7 120 75 +0.98 +2 11/07 07 57.6 +14 13 0.06 1.01 17.1 70.9 106 35 -0.89 +21 11/11 09 00.6 +16 12 0.07 1.00 17.8 80.5 96 8 -0.48 +36 11/15 09 46.7 +16 57 0.08 0.99 18.3 86.0 89 50 -0.12 +46

Minor Planet Bulletin 44 (2017) 360

(190208) 2006 AQ (Oct-Dec, H = 18.2) 3361 Orpheus (Oct-Nov, H = 19.0) This asteroid needs an extensive campaign involving observers at Wisniewski (1991), Polishook (2012), and Skiff (2013) all well-separated longitudes producing high-precision photometry. reported a period of about 3.5 h for this 0.5 km NEA. If caught Warner (2014) reports this as a possible “very wide binary”, one early on, mid-October, here is another excellent chance to find H- where the primary period is very long (182 h, A = 0.25 mag) with G parameters. a short period (2.62 h, A = 0.08 mag) lightcurve superimposed. Confirmation, or not, of the initial discovery is needed. Be careful DATE RA Dec ED SD V α SE ME MP GB ------about using a combined data set that spans more than a month or 10/15 02 20.3 +09 49 0.21 1.20 16.7 12.5 165 108 -0.24 -47 so. Changes in the lightcurve due to changing viewing aspect 10/20 02 15.3 +07 41 0.18 1.17 16.2 8.0 171 175 +0.00 -50 10/25 02 07.8 +04 50 0.15 1.15 15.7 6.6 172 122 +0.24 -53 could lead to false conclusions. 10/30 01 57.5 +01 02 0.13 1.12 15.6 12.0 166 58 +0.70 -58 11/04 01 43.5 -04 00 0.11 1.09 15.4 21.0 157 18 +1.00 -64 DATE RA Dec ED SD V α SE ME MP GB 11/09 01 24.3 -10 46 0.09 1.07 15.3 32.8 144 96 -0.70 -72 ------11/14 00 57.0 -19 45 0.08 1.04 15.3 47.8 129 159 -0.19 -83 10/01 02 32.2 +29 32 0.28 1.23 17.2 31.2 141 95 +0.77 -28 11/19 00 16.0 -31 12 0.07 1.01 15.5 66.4 110 108 +0.00 -81 10/11 03 10.2 +36 55 0.22 1.18 16.7 34.1 139 39 -0.67 -18 11/24 23 10.6 -43 48 0.06 0.99 16.0 88.3 88 45 +0.25 -64 10/21 04 10.0 +45 02 0.19 1.13 16.4 39.9 133 141 +0.02 -5 11/29 21 28.6 -53 25 0.06 0.96 17.2 111.1 65 63 +0.73 -45 10/31 05 43.2 +51 08 0.16 1.09 16.3 47.9 125 103 +0.79 +11 11/10 07 35.4 +51 07 0.16 1.07 16.4 56.0 116 36 -0.59 +27 11/20 09 03.1 +45 21 0.16 1.06 16.6 61.3 110 122 +0.02 +42 (138852) 2000 WN10 (Nov, H = 20.2, PHA) 11/30 09 55.6 +37 57 0.18 1.06 16.8 62.5 108 119 +0.82 +52 The estimated diameter of this NEA is 270 meters. Pravec et al. 12/10 10 24.6 +31 16 0.19 1.07 16.9 59.9 110 25 -0.53 +58 (2011), Skiff et al. (2009), and Warner (2016) all found a period of 12/20 10 38.7 +25 56 0.21 1.09 17.0 54.4 116 132 +0.03 +60 12/30 10 41.8 +21 53 0.23 1.13 17.0 46.6 124 100 +0.86 +60 about 4.46 h. To date, the amplitude has been fairly large, at least 0.38 mag. Will it be so this time around? (162004) 1991 VE (Nov, H = 18.2) Pravec et al. (2012) and Warner (2015) both report a period of DATE RA Dec ED SD V α SE ME MP GB ------about 13.5 h for this 700 meter NEA. 11/01 05 33.8 -57 16 0.15 1.03 18.7 73.2 98 84 +0.87 -33 11/04 04 45.4 -52 37 0.14 1.04 18.3 66.0 107 69 +1.00 -40 DATE RA Dec ED SD V α SE ME MP GB 11/07 04 02.2 -46 02 0.13 1.05 18.0 57.9 116 68 -0.89 -48 ------11/10 03 26.0 -37 50 0.13 1.07 17.7 49.5 125 91 -0.59 -56 11/05 20 07.5 -38 54 0.19 0.96 17.9 94.8 74 115 -0.99 -31 11/13 02 56.8 -28 45 0.13 1.08 17.6 41.8 133 124 -0.28 -62 11/07 20 48.3 -35 41 0.20 0.98 17.7 87.7 81 134 -0.89 -38 11/16 02 33.7 -19 41 0.14 1.10 17.5 35.7 140 152 -0.06 -65 11/09 21 22.4 -32 03 0.21 1.00 17.7 81.3 87 153 -0.70 -45 11/19 02 15.7 -11 20 0.15 1.11 17.6 32.2 143 142 +0.00 -65 11/11 21 50.4 -28 23 0.22 1.02 17.7 75.8 92 166 -0.48 -50 11/22 02 01.7 -04 05 0.16 1.12 17.8 31.0 144 109 +0.11 -61 11/13 22 13.2 -24 55 0.24 1.04 17.7 71.1 96 157 -0.28 -55 11/25 01 51.0 +01 59 0.18 1.13 18.1 31.6 143 73 +0.34 -58 11/15 22 32.0 -21 45 0.26 1.06 17.8 67.1 99 138 -0.12 -58 11/28 01 42.7 +07 00 0.20 1.15 18.4 33.2 141 35 +0.63 -54 11/17 22 47.5 -18 55 0.28 1.08 17.9 63.8 101 118 -0.02 -60 11/19 23 00.7 -16 24 0.31 1.10 18.0 61.1 103 98 +0.00 -62 (444584) 2006 UK (Oct-Nov, H = 20.2) 11/21 23 11.9 -14 11 0.33 1.12 18.1 58.8 105 78 +0.06 -63 11/23 23 21.6 -12 12 0.35 1.13 18.3 57.0 106 57 +0.18 -64 There is no period reported in the LCDB. The estimated diameter is 270 meters, so it’s probable that the period is going to be more (457768) 2009 KN4 (Oct-Dec, H = 18.3) than 2 hours. The estimated diameter is 650 meters; there is no lightcurve period listed in the LCDB. The large phase angles in October could make DATE RA Dec ED SD V α SE ME MP GB ------lightcurve analysis difficult because of deep shadowing effects. 10/25 02 36.3 +29 24 0.21 1.20 18.1 16.2 160 133 +0.24 -28 10/28 02 32.6 +29 55 0.19 1.17 17.7 15.0 162 99 +0.51 -28 DATE RA Dec ED SD V α SE ME MP GB 10/31 02 27.4 +30 28 0.16 1.15 17.3 14.3 163 63 +0.79 -28 ------11/03 02 19.9 +31 08 0.13 1.12 16.8 14.5 164 28 +0.98 -28 10/20 18 28.0 +19 47 0.21 0.97 18.1 90.4 77 72 +0.00 +14 11/06 02 08.6 +31 58 0.10 1.09 16.4 16.3 162 35 -0.95 -28 10/25 19 03.8 +26 38 0.20 0.99 17.8 84.6 84 49 +0.24 +9 11/09 01 49.8 +33 04 0.08 1.06 15.9 20.5 158 77 -0.70 -28 10/30 19 46.6 +33 13 0.20 1.02 17.5 77.3 91 57 +0.70 +4 11/12 01 13.5 +34 31 0.06 1.04 15.3 29.1 149 120 -0.38 -28 11/04 20 36.4 +38 47 0.20 1.04 17.4 69.4 100 83 +1.00 -1 11/15 23 43.7 +35 00 0.03 1.01 14.7 49.0 130 143 -0.12 -26 11/09 21 31.0 +42 38 0.21 1.07 17.3 61.5 108 113 -0.70 -6 11/18 20 07.6 +17 59 0.02 0.98 15.6 101.7 77 78 +0.00 -8 11/14 22 25.8 +44 32 0.23 1.11 17.3 54.3 115 128 -0.19 -11 11/19 23 16.1 +44 44 0.25 1.14 17.4 48.1 121 114 +0.00 -15 (333888) 1998 ST4 (Oct-Dec, H = 16.4) 11/24 23 59.3 +43 49 0.28 1.17 17.6 43.1 126 81 +0.25 -18 11/29 00 35.0 +42 16 0.32 1.21 17.8 39.3 129 44 +0.73 -21 At 1.6 km, this is one of the larger NEAs in this quarter’s 12/04 01 04.3 +40 30 0.35 1.25 18.0 36.6 131 56 -1.00 -22 collection. The rotation period is unknown.

(99907) 1989 VA (Oct-Dec, H = 17.9) DATE RA Dec ED SD V α SE ME MP GB Pravec et al. (1997) reported a period of 2.5 h. That’s 20 years ------10/01 00 24.8 +23 11 0.60 1.58 17.0 12.6 160 66 +0.77 -39 ago. It often gets brighter than V = 17.0, so it’s curious that it has 10/11 00 16.3 +22 07 0.53 1.51 16.6 12.6 161 77 -0.67 -40 not been observed since, except that the U = 3 rating in the LCDB 10/21 00 07.8 +20 03 0.47 1.43 16.4 16.8 155 142 +0.02 -42 10/31 00 02.1 +17 06 0.42 1.37 16.3 23.6 147 30 +0.79 -44 lead observers to believe that additional data were not needed. 11/10 00 01.5 +13 35 0.39 1.31 16.3 31.3 137 120 -0.59 -48 11/20 00 08.0 +09 52 0.37 1.25 16.3 38.7 128 110 +0.02 -52 DATE RA Dec ED SD V α SE ME MP GB 11/30 00 22.6 +06 17 0.35 1.20 16.3 45.3 120 13 +0.82 -56 ------12/10 00 45.6 +03 05 0.34 1.17 16.3 50.6 114 152 -0.53 -60 10/10 06 45.1 +39 18 0.38 1.11 18.3 63.0 97 33 -0.77 +16 12/20 01 16.7 +00 24 0.33 1.14 16.3 54.3 110 91 +0.03 -62 10/17 06 29.3 +36 15 0.32 1.13 17.8 57.2 107 74 -0.08 +12 12/30 01 55.4 -01 37 0.33 1.13 16.3 56.2 108 29 +0.86 -60 10/24 06 04.5 +31 42 0.27 1.15 17.2 49.0 119 162 +0.16 +5 10/31 05 27.0 +24 20 0.22 1.16 16.4 37.3 135 100 +0.79 -6 11/07 04 35.2 +12 39 0.19 1.16 15.6 22.1 154 15 -0.89 -23 (163696) 2003 EB50 (Oct-Dec, H = 16.4, PHA) 11/14 03 33.7 -02 28 0.18 1.16 15.4 17.9 159 128 -0.19 -44 Warner observed this NEA at three apparitions (2013, 2015, 11/21 02 34.6 -15 53 0.20 1.15 16.1 33.4 140 121 +0.06 -64 2017). The data from 2013 led to a period of 27 h with the 11/28 01 48.0 -24 27 0.24 1.13 16.9 47.7 122 38 +0.63 -77 12/05 01 15.2 -29 10 0.29 1.11 17.5 57.8 108 86 -0.97 -84 possibility of tumbling. The data from 2015 and 2017 resulted in a 12/12 00 53.1 -31 45 0.34 1.08 18.0 65.1 97 148 -0.33 -85 period of about 62.5 h with large amplitudes and no obvious signs of tumbling. High-precision observations with dense observations every night (at least 10-15 spread out over 6 or more hours, not a

Minor Planet Bulletin 44 (2017) 361 handful over 1-2 hours) will be needed. Long period objects, (418849) 2008 WM64 (Dec-Jan, H = 20.7, PHA) especially if there is a possibility of tumbling, need a healthy This NEA has no reported period in the LCDB. The diameter is amount of data and lots of patience. estimated to be about 215 meters.

DATE RA Dec ED SD V α SE ME MP GB DATE RA Dec ED SD V α SE ME MP GB ------10/01 12 55.9 -51 05 0.56 0.76 18.1 98.3 48 93 +0.77 +12 12/15 08 45.7 -39 38 0.08 1.01 17.9 73.1 102 86 -0.10 +2 10/11 12 30.5 -54 47 0.46 0.77 18.1 105.5 48 111 -0.67 +8 12/17 08 37.5 -31 55 0.07 1.01 17.2 66.3 110 105 -0.02 +6 10/21 11 51.1 -55 58 0.35 0.82 17.9 110.3 50 56 +0.02 +6 12/19 08 26.4 -19 17 0.05 1.01 16.3 55.2 122 130 +0.01 +11 10/31 10 58.4 -53 13 0.25 0.88 17.3 110.6 56 118 +0.79 +6 12/21 08 10.9 +01 30 0.04 1.02 15.4 37.9 141 162 +0.07 +18 11/10 09 48.0 -41 51 0.16 0.95 15.9 101.2 70 62 -0.59 +9 12/23 07 48.4 +29 26 0.04 1.02 14.8 23.0 156 150 +0.19 +24 11/20 08 04.1 -02 23 0.09 1.03 13.6 63.1 112 129 +0.02 +15 12/25 07 14.2 +53 40 0.05 1.02 15.4 30.9 148 113 +0.36 +25 11/30 05 54.7 +44 14 0.14 1.11 13.5 25.9 151 74 +0.82 +9 12/27 06 20.6 +68 24 0.06 1.03 16.3 42.6 135 86 +0.57 +22 12/10 04 21.6 +55 42 0.24 1.19 14.9 27.4 146 89 -0.53 +4 12/29 05 00.2 +75 55 0.08 1.03 17.1 50.4 126 69 +0.77 +20 12/20 03 37.6 +57 28 0.36 1.28 16.0 30.9 138 126 +0.03 +1 12/31 03 22.0 +78 53 0.09 1.03 17.7 55.4 120 62 +0.93 +18 12/30 03 22.3 +57 12 0.49 1.36 16.9 32.9 131 43 +0.86 +0 01/02 01 56.7 +79 18 0.11 1.04 18.2 58.7 116 67 +1.00 +17

3200 Phaethon (Oct-Dec, H = 14.6, PHA) (294739) 2008 CM (Nov-Dec, H = 15.2) Period determinations of about 3.6 hours go back at least two The period of this NEA is close to 3.0 h; the synodic period has decades. Hanus et al. (2016) derived a shape and spin axis model varied about 0.05 h on either side. The estimated diameter is about for the asteroid. That does not mean you should neglect this 5 km 1.1 km. As often happens with NEAs, the phase angles during an NEA. Additional data can help find YORP acceleration and/or apparition are very large and the solar elongations not so much so. improve the quality of the current pole solution. DATE RA Dec ED SD V α SE ME MP GB DATE RA Dec ED SD V α SE ME MP GB ------11/01 13 56.0 +52 53 0.52 0.93 18.5 81.5 68 125 +0.87 +62 10/01 06 30.2 +33 25 1.57 1.88 18.3 32.1 91 145 +0.77 +11 11/11 13 21.1 +47 34 0.46 0.93 18.3 83.5 69 57 -0.48 +69 10/11 06 41.9 +33 40 1.36 1.80 17.9 33.2 99 18 -0.67 +13 11/21 12 47.8 +39 15 0.40 0.95 18.0 84.0 72 91 +0.06 +78 10/21 06 52.1 +33 58 1.15 1.72 17.5 33.9 106 119 +0.02 +15 12/01 12 16.2 +26 58 0.35 0.97 17.7 81.7 78 136 +0.90 +82 10/31 07 00.3 +34 25 0.93 1.62 16.9 34.0 114 119 +0.79 +17 12/11 11 44.3 +10 13 0.31 1.01 17.3 75.8 87 7 -0.43 +67 11/10 07 05.5 +35 07 0.72 1.51 16.2 33.3 123 27 -0.59 +18 12/21 11 09.1 -09 20 0.30 1.06 17.1 67.0 97 126 +0.07 +46 11/20 07 04.9 +36 18 0.52 1.40 15.3 31.4 133 146 +0.02 +18 12/31 10 27.7 -27 06 0.32 1.11 17.1 58.2 106 96 +0.93 +26 11/30 06 50.9 +38 37 0.33 1.27 13.9 27.1 144 84 +0.82 +16 12/10 05 34.0 +44 07 0.15 1.12 11.6 19.1 158 79 -0.53 +6 12/20 22 29.4 +00 49 0.09 0.96 13.0 103.4 72 53 +0.03 -46

(140158) 2001 SX169 (Nov-Dec, H = 18.3) There is no period in the LCDB for this NEA. The WISE survey (Mainzer et al., 2011) found a diameter of 566 meters. Using H = 18.2, they found an albedo of pV = 0.289.

DATE RA Dec ED SD V α SE ME MP GB ------11/01 04 44.2 +14 38 0.45 1.39 18.4 23.4 146 75 +0.87 -20 11/08 04 41.8 +13 36 0.38 1.34 17.8 19.3 153 28 -0.80 -21 11/15 04 35.4 +12 15 0.32 1.29 17.2 14.4 161 124 -0.12 -23 11/22 04 23.9 +10 29 0.26 1.24 16.5 10.0 167 147 +0.11 -26 11/29 04 05.6 +08 05 0.21 1.19 16.0 11.3 166 57 +0.73 -31 12/06 03 38.1 +04 45 0.17 1.14 15.7 21.2 155 54 -0.92 -39 12/13 02 56.7 -00 01 0.13 1.09 15.6 37.2 138 158 -0.24 -49 12/20 01 54.5 -06 49 0.11 1.03 15.6 59.9 115 98 +0.03 -65 12/27 00 24.5 -15 12 0.09 0.98 16.2 90.2 85 18 +0.57 -77

(276703) 2004 BL11 (Dec, H = 19.2) The effective diameter of this NEA is about 0.5 km. There is no period reported in the LCDB. Unfortunately, the asteroid stays close to the galactic plane, meaning dense star fields and difficulties getting good photometry.

DATE RA Dec ED SD V α SE ME MP GB ------12/20 07 14.9 -32 41 0.18 1.09 17.5 51.3 120 127 +0.03 -10 12/21 07 02.0 -29 55 0.19 1.10 17.5 47.7 124 129 +0.07 -11 12/22 06 50.5 -27 15 0.19 1.11 17.5 44.3 128 127 +0.12 -12 12/23 06 40.3 -24 42 0.20 1.12 17.6 41.2 131 121 +0.19 -13 12/24 06 31.2 -22 17 0.21 1.14 17.6 38.5 134 113 +0.27 -14 12/25 06 23.1 -20 00 0.22 1.15 17.6 36.0 137 103 +0.36 -15 12/26 06 15.8 -17 52 0.23 1.16 17.7 33.9 139 92 +0.46 -16 12/27 06 09.3 -15 52 0.24 1.17 17.8 32.0 141 80 +0.57 -16 12/28 06 03.4 -14 00 0.25 1.19 17.8 30.5 142 67 +0.67 -17 12/29 05 58.1 -12 15 0.26 1.20 17.9 29.1 144 54 +0.77 -17

Minor Planet Bulletin 44 (2017) 362

INDEX TO VOLUME 44 Foylan, M. “Lightcurve and Rotation Period for Minor Planet (7774) 1992 UU2” 92. Alton, K.B. “CCD Lightcurves for Main-belt Asteroids 423 Diotima and 925 Alphonsina” 188–189. Foylan, M., Durkee, R.I. “A Revised Rotation Period for Minor Planet 2420 Čiurlionis” 91–92. Àlvarez, E.M. “Certainties, Question Marks and Voids in the Present-day Data Concerning the Rotation Period of Asteroids” Franco, L., Baj, G., Tinella, V., Bachini, M., Succi, G., 167–171. Casalnuovo, G.B., Bacci, P. “Rotation Periods for Three Main Belt Asteroids” 311–312. Apostolovska, G., Kostov, A., Donchev, Z. Ovcharov, E. “Lightcurve of 1563 Noel at Low Phase Angle” 143. Franco, L., Klinglesmith, D.A. III, Pilcher, F. “Rotation Period for 1218 Aster” 185–186. Benishek, V. “Lightcurves and Rotation Periods for Six Asteroids” 67–69. Franco, L., Marchini, A. “Rotation Periods for 1751 Herget, 2022 West, and (23997) 1999 RW27” 93–94. Benishek, V. “Lightcurves and Synodic Rotation Periods for 3067 Akhmatova, 5397 Vojislava, 5823 Oryo, 5909 Nagoya, and Franco, L., Scardella, M., Tomassini, A., Franceschini, F., Pierri, (23997) 1999 RW27” 151–153. F., Marchini, A. “Period Determination for 703 Noemi” 247–248.

Benishek, V., Pilcher, F. “Lightcurve and Rotation Period Hayes-Gehrke, M.N., Arrington, K., Brady, J., Christian, S., Determination for 1773 Rumpelstilz” 262. Ginsburg, S., McLeod-Campbell, D., Musial, C., Pham, A., Woodward, D. “Lightcurve Analysis for 2142 Landau” 306–307. Benishek, V., Pilcher, F., Montaigut, R., Leroy, A., Carbognani, A., Pravec, P. “3792 Preston: Another Two-Period Case” 149– Hayes-Gehrke, M.N., Caffes, R., Gibson, A., Honer, A., Hunter, 151. R., Paul, T., Quimby, C., Riffe, T., Roberts, M., Schemmel, J., Unaegbu, U., Wilton, Z. “Lightcurve for Asteroid 4404 Enirac” Binzel, R.P. “Editorial Announcements: MPB Volume 44” 1. 309.

Brincat, S.M. “Lightcurve Analysis for Three Main-Belt Hayes-Gehrke, M.N., de La Beaujardiere, J., Kotgire, P., Piel, A., Asteroids” 1–2. King, M., Tran, K., Kenyon, J., Hagen, D., Fulling, L., Walters, J., Acuna, A. “Lightcurve Analysis for Near-Earth Asteroid (138404) Brincat, S.M. “Rotation Period Determination of Asteroids 6199 2000 HA24” 310. Yoshiokayayoi and 9671 Hemera” 199–200. Hayes-Gehrke, M., Linko, D., Bhasin, R., Johnson, J., Bermudez, Brincat, S.M., Grech, W. “Photometric Observations of Main-Belt Asteroids 1990 Pilcher and 8443 Svecicia” 287–288. B., Fedorenko, I., Tillis, K., Villar, N. “Lightcurve and Rotation Period for Minor Planet 2504 Gaviola” 308. Brines, P., Lozano, J., Rodrigo, O., Fornas, A., Herrero, D., Mas Hergenrother, C., Hill, D. “Target Asteroids! Observing V., Fornas, G., Carreño, A., Arce, E. “Sixteen Asteroids Campaigns” Lightcurves at Asteroids Observers (OBAS) – MPPD: 2016 June– 2017 January–March 72–74. November” 145–149. 2017 April–June 158–160.

Brown, J.E. Jr., Linder, T., Puckett, A., Holmes R. “Period Hess, K., Bruner, M., Ditteon, R. “Asteroid Lightcurve Analysis at Determination of Main-Belt Asteroid (26274) 1998 RH75” 111. the Oakley Southern Sky Observatory: 2015 February – March” 3–5. Carbognani, A. “Asteroids Lightcurves Analysis at OAVdA: 2016 January–October” 52–57. Hills, K. “Asteroid Lightcurve Analysis at Tacande Observatory: 3679 Condruses, 4871 Riverside, 4895 Embla, and 5403 Casalnuovo, G.B. “Lightcurve Analysis for Ten Main Belt Takachiho” 114–115. Asteroids” 178–181. Klinglesmith, D.A. III, “Asteroid Photometry Results from Coley, D. “Follow-up Observations of 788 Hohensteina” 261. Etscorn Observatory” 69–72.

Davalos, J.A.G., Silva, J.S., Tamayo, F.J., Schuster, J.W., Alvarez, Klinglesmith, D.A. III, “Asteroids Observed from Estcorn F.I. “Rotation Period for (332660) 2008 WL7” 298. Observatory” 345–348.

DeGraff, D.R. “Stull Observatory Lightcurve Observations: 1998– Klinglesmith, D.A. III, “Spin-Shape Model Lightcurves” 127– 2002” 350–354. 129.

Deshmukh, S. “Measurements of 100 ‘Critical’ Minor Planets Klinglesmith, D.A. III, Hendricks, S., Kimber, C., Madden, K. from NEAT Archive” 265–269. “CCD Asteroid Photometry From Etscorn Observatory” 244–246.

Ferrero, A. “Rotational Period of Three Main-Belt Asteroids” 142. Kosiarek, M., Nisley, I., Patra, K., Hatano, R., Bates, H., Chavez, E., Kosiarek, J.L., Kumari, S. “Rotation Period of Asteroid 3494 Foylan, M. “Lightcurve and Rotation Period for Minor Planet Purple Mountain” 171–172. 1715 Salli” 11.

Minor Planet Bulletin 44 (2017) 363

Kretlow, M., Jahn, J. “Lightcurve Analysis of (222317) 2000 4296 van Woerkom: A Newly Discovered Asynchronous Binary” TE1” 144. 242–243.

Lang, K. “Lightcurves from the Archive: 1090 Sumida, 2284 San Odden, C.E., Durrett, O.N., Dolan, P.E., Wang, T. “The Juan, and 3493 Stepanov” 7–8. Lightcurve and Rotation Period of Asteroid 9414 Masamimurakami” 205. Linder, T.R., Puckett, A., Holmes, R., Nowinski, M., Hardersen, P., Haislip, J., Reichart, D. “Near Earth Asteroid Rotational Odden, C.E, Jusuf, J.M., Keefe, O.R., Wang, A., Zaeder, E.A. Analysis by Astronomical Research Institute: 2015 November thru “The Rotation Periods of Asteroids 4668 Rayjay, 5152 Labs, 6581 2016 August” 95–98. Sobers, and 14917 Taco” 181–182.

Linville, D., Jiang, H., Michalik, D., Wilson, S., Ditteon, R. Oey, J., Williams, H., Groom, R. “Lightcurve Analysis of “Lightcurve Analysis of Asteroids Observed at the Oakley Asteroids from BMO and DRO in 2015” 200–204. Southern Sky Observatory: 2016 July–October” 173–176. Oey, J., Williams, H., Groom, R., Pray, D., Benishek, V. Lozano, J., Flores, A., Mas, V., Fornas, G. “Severn Near-Earth “Lightcurve Analysis of Binary and Potential Binary Asteroids in Asteroids at Asteroids Observers (OBAS) – MPPD: 2016 June– 2015” 193–199. November” 108–111. Papini, R., Marchini, A., Salvaggio, F. “Rotation Period Macías, A.A. “3637 O’Meara: New Binary Candidate” 59–60. Determination of Asteroids 5059 Saroma and 5399 Awa” 153– 155. Macías, A.A, “Density and Axis-size Relationship of Five Main- belt Asteroids: 2017 January–March” 276–279. Papini, R., Marchini, A., Salvaggio, F. “Rotation Period Determination of Asteroids (8360) 1990 FD1 and (11386) 1998 Macías, A.A. “Lightcurve Analysis for Nine Main-Belt Asteroids. TA18” 63–65. Rotation Period and Physical Parameters from APT Observatory Group: 2016 October–December” 139–141. Pilcher, F. “Call for Observations” 90.

Macías, A.A. “Lightcurve Analysis from APT Observatory Group Pilcher, F. “General Report of Position Observations by the ALPO for Nine Mainbelt Asteroids: 2016 July–September. Rotation Minor Planets Section for the Year 2016” 263–264. Period and Physical Parameters” 60–63. Pilcher, F. “Lightcurves of 131 Vala and 612 Veronika during Marchini, A., Ballini, E., Chianese, E., Maggioni, E., Scali, S., their 2017 Apparitions” 317–318. Trefoloni, B., Papini, R., Salvaggio, F. “Rotation Period Determination for 2411 Zellner, 5293 Bentengahama, and 9148 Pilcher, F. “Minor Planets at Unusually Favorable Elongations in Boriszaitsev” 274–276. 2017” 5–7.

Marchini, A., Palmas, T., Franco, L., Papini, R., Salvaggio, F. Pilcher, F. “Rotation Period Determinations for 46 Hestia, 118 “Rotation Period Determination for 4963 Kanroku” 66–67. Peitho, 333 Badenia, 356 Liguria, and 431 Nephele” 294–297.

Marchini, A., Papini, R., Salvaggio, F. “Rotation Period Pilcher, F. “Rotation Period Determinations for 49 Pales, 96 Determination for 3077 Henderson and 12044 Fabbri” 137–138. Aegle, 106 Dione, 375 Ursula, and 576 Emanuela” 249–251.

Marchini, A., Papini, R., Salvaggio, F. “Rotation Period Pilcher, F. “Rotation Period Determinations for 392 Wilhelmina Determination for 3892 Dezso and 14339 Knorre” 349–350. and 864 Aase” 9.

Mizoguchi, T., Tanaka, A., Nakata, A., Hirono, K., Moriuchi, S., Pilcher, F. “Rotation Period Determinations for 396 Aeolia, 398 Nakamura, S., Watanabe, A., Koyago, H., Koyama, I., Morimoto, Admete, 422 Berolina, and 555 Norma” 112–114. K., Nakai, M., Kitora, S., Tanigawa, T. “The Lightcurve Period for the Asteroid 201 Penelope” 190. Pilcher, F., Benishek, V. “Rotation Period Determination for 467 Laura” 183. Monteiro, F., Silva, J.S., Lazzaro, D., Arcoverde, P., Medeiros, H., Souza, R., Rodrigues, T. “Lightcurve Analysis for Ten Near-Earth Pilcher, F., Franco, L., Odden, C., Marler, S., Paris, L., Ward, Asteroids” 20–22. N.S., Yung, V. “Rotation Period Determination for 213 Lilaea” 303. (MPB staff) “Author’s Guide” 81–85. Pilcher, F., Franco, L., Pravec, P. “299 Thora and 496 Gryphia: Noschese, A., Vecchione, A., D’Avino, L., Izzo, L. “Lightcurve Two More Very Slowly Rotating Asteroids” 270–274. Analysis for Minor Planet 703 Noemi” 177–178. Pilcher, F., Franco, L., Pravec, P. “319 Leona and 341 California – Odden, C.E., Caso, M., Dettorre, C., Dial, P.J., Hoang, K., Two Very Slowly Rotating Asteroids” 87–90. Hughes, R., Lazar, T.T., Morss, P.P., Mundra, A.R. “Lightcurve Analysis of 1773 Rumpelstilz and 2040 Chalonge” 219–220. Pilcher, F., Marciniak, A., Kaminski, K., Horbowicz, J., Skrzypek, J., Oey, J., Ogloza, W. “Rotation Period Determination for 397 Odden, C.E., Caso, M., Dettorre, C., Dial, P.J., Hoang, K., Lazar, Vienna” 316. T.T., Morss, P.P., Mundra, A.R., Naiyapatana, A., Rooney, M., Pravec, P., Benishek, V., Klinglesmith, D., Pilcher, F. “Asteroid Pilcher, F., Marciniak, A., Oey, J. “Rotation Period Determination for 393 Lampetia” 238. Minor Planet Bulletin 44 (2017) 364

Polakis, T., Skiff, B.A. “Lightcurve Analysis for 341 Califorina, Warell, J. “Lightcurve Observations of Nine Main-Belt Asteroids” 594 Mireille, 1115 Sabauda, 1504 Lappeenranta, and 1926 304–305. Demiddelaer” 299–302. Warner, B.D. “Asteroid-Deepsky Appulses in 2017” 10. Reshetnyk, V., Godunova, V., Andreev, M., Polyakov, V. “Lightcurve Analysis for Near-Earth Asteroid 2015 SZ2” 65. Warner, B.D. “Asteroid Lightcurve Analysis at CS3-Palmer Divide Station” Ruthroff, J.C. “The Rotation Period of 10041 Parkinson” 288– 2016 July–September 12–19. 289. 2016 October–December 116–120. 2016 December thru 2017 March 213–219. Sada, P.V., Olguín, L., Saucedo, J.C., Loera-González, P., Cantú- 2017 April thru June 289–294. Sánchez, L., Garza, J.R., Ayala-Gómez, S.A., Avilés, A., Pérez- Tijerina, E., Navarro-Meza, S., Silva, J.S., Reyes–Ruiz, M., Warner, B.D. “Lightcurve Analysis of Two Near-Earth Asteroids: Segura-Sosa, J., López-Valdivia, R., Álvarez-Santana, F. “Results 2010 VB1 and 2014 JO25” 327–330. of the 2016 Mexican Asteroid Photometry Campaign” 239–242. Warner, B.D. “Near-Earth Asteroid Lightcurve Analysis at CS3- Salvaggio, F., Marchini, A., Papini, R. “Asteroid Lightcurve Palmer Divide Station” Analysis at Astronomical Observatory – University of Siena 2016 July–September 22–36. (Italy) 2016 October–December 98–107. 2016 May–September” 57–58. 2016 December thru 2017 April 223–237. 2016 October–December” 155–156. 2017 April thru June 335–344.

Salvaggio, F., Marchini, A., Papini, R. “Rotation Period Warner, B.D., Benishek, V., Harris, A.W. “1943 Anteros: A Determination for 3760 Poutanen and 14309 Defoy” 354–355. Possible Near-Earth Binary Asteroid” 186–188.

Salvaggio, F., Marchini, A., Papini, R. “Rotation Period Warner, B.D., Harris, A.W., Ďurech, J., Benner, L.A.M. Determination for 9671 Hemera” 248–249. “Lightcurve Photometry Opportunities” 2017 January–March 74–80. Schmidt, R.E. “Near-IR Minor Planet Photometry from Burleith 2017 April–June 160–164. Observatory” 191–192. 2017 July–September 279–284. 2017 October–December 355–361. Şonka, A.B., Popescu, M., Nedelcu, D.A, Gherase, R.M, Vass, G. “Photometric Observations of the Near-Earth Asteroids 326683 Warner, B.D., Harris, A.W., Macías, A.A., Oey, J. “Lightcurve (2002 WP) and 2016 LX48” 176–177. Analysis of NEA (190166) 2005 UP156: A New Fully- Synchronous Binary” 324–325. Stephens, R.D. “Asteroids Observed from CS3” 2016 July–September 49–52. Warner, B.D, Macías, A.A., Ballano, A.S. “Lightcurve Analysis of 2016 October–December 120–122. the Near-Earth Asteroid 2016 NL15” 157–158. 2017 January–March 257–258. 2017 April–June 321–323. Warner, B.D., Macías, A.A., Benishek, V., Oey, J., Groom, R. “Lightcurve Analysis of the Near-Earth Asteroid 6063 Jason” Stephens, R.D. “Lightcurve Analysis of Trojan Asteroids at the 325–326. Center for Solar System Studies 2016 October–December” 123– 125. Warner, B.D., Pravec, P., Kusnirak, P., Benishek, V., Ferrero, A. “Preliminary Pole and Shape Models for Three Near-Earth Stephens, R.D., Coley, D.R. “Lightcurve Analysis of Trojan Asteroids” 206–212. Asteroids at the Center for Solar System Studies” 2017 January–March 252–257. Warner, B.D., Stephens, R.D. “Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies” Stephens, R.D., French, L.M., James, D., Rohl, D., Warner, B.D. 2016 December thru 2017 April 220–222. “Main-Belt Asteroid Lightcurves from Cerro Tololo Inter- 2017 April thru July 331–334. American Observatory – 2016 April” 42–49. Warner, B.D., Stephens, R.D., Coley, D.R. “Lightcurve Analysis Stephens, R.D., Warner, B.D. “Lightcurve Analysis of L4 Trojan of Hilda Asteroids at the Center for Solar System Studies” Asteroids at the Center for Solar System Studies” 2016 June–September 36–41. 2017 April–June 312–316. 2016 September–December 130–137.

Stephens, R.D., Warner, B.D. “(24465) 2000 SX155: A New Washburn, K. Ditteon, R. “Lightcurve Analysis of Asteroids Binary Hungaria” 126–127. Observed at the Oakley Southern Sky Observatory: 2016 October” 184–185. Stephens, R.D., Warner, B.D., Macías, A.A., Benishek, V. “(24495) 2001 AV1 – A Suspected Very Wide Binary” 319–320. Zeigler, K., Hanshaw, B., Gass, J. “Photometric Observations of Asteroids 4742 Caliumi, 5267 Zegmott, (18429) 1994 AO1, Tan, H., Li, B., Gao, X. “The Rotation Period of 1117 Reginita” (26421) 1999 XP113, and (27675) 1981 CH” 259–260. 307.

Minor Planet Bulletin 44 (2017) 365

IN THIS ISSUE Number Name EP Page Number Name EP Page 1998 Titius 35 321 13504 1988 RV12 45 331 2042 Sitarski 18 304 14309 Defoy 68 354 This list gives those asteroids in this issue for 2142 Landau 20 306 14339 Knorre 63 349 which physical observations (excluding 2329 Orthos 49 335 15440 1998 WX4 26 312 astrometric only) were made. This includes 2383 Bradley 18 304 15527 1999 YY2 26 312 lightcurves, color index, and H-G 2501 Lohja 25 311 15540 2000 CF18 45 331 determinations, etc. In some cases, no specific 2504 Gaviola 22 308 16206 2000 CL39 18 304 results are reported due to a lack of or poor 2544 Gubarev 64 350 16562 1992 AV1 3 289 2572 Annschnell 35 321 17014 1999 CY96 3 289 quality data. The page number is for the first 2920 Automedon 26 312 20713 1999 XA32 64 350 page of the paper mentioning the asteroid. EP is 2959 Scholl 45 331 22058 2000 AA64 45 331 the “go to page” value in the electronic version. 3000 Leonardo 18 304 23481 1991 GT4 64 350 3022 Dobermann 3 289 24495 2001 AV1 33 319 Number Name EP Page 3028 Zhangguoxi 64 350 24691 1990 RH3 18 304 46 Hestia 8 294 3193 Elliot 35 321 27000 1998 BO44 3 289 118 Peitho 8 294 3254 Bus 45 331 27097 1998 UM26 3 289 131 Vala 31 317 3266 Bernardus 3 289 51122 2000 HN35 3 289 213 Lilaea 17 303 3290 Azabu 45 331 52586 1997 PB 3 289 314 Rosalia 64 350 3709 Polypoites 26 312 56473 2000 GY108 3 289 333 Badenia 8 294 3760 Poutanen 68 354 68348 2001 LO7 49 335 341 California 13 299 3892 Dezso 63 349 100926 1998 MQ 49 335 356 Liguria 8 294 4008 Corbin 35 321 106589 2000 WN107 49 335 397 Vienna 30 316 4060 Deipylos 26 312 132450 2002 HT1 3 289 431 Nephele 8 294 4068 Menestheus 26 312 138404 2000 HA24 24 310 459 Signe 59 345 4404 Enirac 23 309 141056 2001 XV4 49 335 594 Mireille 13 299 4464 Vulcano 35 321 143404 2003 BD44 49 335 596 Scheila 3 289 4490 Bambery 3 289 163696 2003 EB50 49 335 611 Valeria 59 345 4833 Meges 26 312 190166 2005 UP156 38 324 612 Veronika 31 317 4974 Elford 18 304 215588 2003 HF2 49 335 901 Brunsia 59 345 5215 Tsurui 64 350 222073 1999 HY1 49 335 939 Isberga 59 345 5471 Tunguska 18 304 247259 2001 RT98 3 289 1016 Anitra 59 345 5653 Camarillo 49 335 332660 2008 WL7 12 298 1022 Olympiada 25 311 5879 Almeria 49 335 388838 2008 EZ5 49 335 1084 Tamariwa 64 350 6009 Yuzuruyoshii 59 345 418094 2007 WV4 49 335 1115 Sabauda 13 299 6063 Jason 39 325 427643 2003 VF1 49 335 1117 Reginita 21 307 6107 Osterbrock 35 321 441987 2010 NY65 49 335 1369 Ostanina 35 321 6493 Cathybennett 3 289 474179 1999 VS6 49 335 1504 Lappeenranta 13 299 6674 Cezanne 3 289 474231 2001 HZ7 49 335 1602 Indiana 25 311 6921 Janejacobs 35 321 475665 2006 VY13 49 335 1656 Suomi 3 289 7174 Semois 45 331 484795 2009 DE47 49 335 1696 Nurmela 35 321 7247 Robertstirling 35 321 2005 GL9 49 335 1748 Mauderli 45 331 7888 1993 UC 49 335 2010 VB1 41 327 1758 Naantali 64 350 8130 Seeberg 45 331 2011 ED78 49 335 1845 Helewalda 64 350 8443 Svecica 1 287 2014 JO25 41 327 1911 Schubart 18 304 8679 Tingstäde 18 304 2014 KF91 49 335 1917 Cuyo 49 335 9829 Murillo 45 331 2017 CS 49 335 1926 Demiddelaer 13 299 10041 Parkinson 2 288 2017 FH101 49 335 1967 Menzel 59 345 11395 1998 XN77 26 312 2017 GM4 49 335 1980 Tezcatlipoca 49 335 11398 1998 YP11 49 335 2017 JA2 49 335 1990 Pilcher 1 287 13186 1996 UM 35 321 2017 MC1 49 335

Minor Planet Bulletin 44 (2017) 366

MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly journal of the Minor Planets Section of the Association of Lunar and Planetary Observers (ALPO). Current and most recent issues of the MPB are available on line, free of charge from: http://www.minorplanet.info/minorplanetbulletin.html Nonmembers are invited to join ALPO by communicating with: Matthew L. Will, A.L.P.O. Membership Secretary, P.O. Box 13456, Springfield, IL 62791-3456 ([email protected]). The Minor Planets Section is directed by its Coordinator, Prof. Frederick Pilcher, 4438 Organ Mesa Loop, Las Cruces, NM 88011 USA ([email protected], assisted by Lawrence Garrett, 206 River Rd., Fairfax, VT 05454 USA ([email protected]). Dr. Alan W. Harris (Space Science Institute; [email protected]), and Dr. Petr Pravec (Ondrejov Observatory; [email protected]) serve as Scientific Advisors. The Asteroid Photometry Coordinator is Brian D. Warner, Palmer Divide Observatory, 446 Sycamore Ave., Eaton, CO 80615 USA ([email protected]).

The Minor Planet Bulletin is edited by Professor Richard P. Binzel, MIT 54-410, 77 Massachusetts Ave, Cambridge, MA 02139 USA ([email protected]). Brian D. Warner (address above) is Associate Editor, and Dr. David Polishook, Department of Earth and Planetary Sciences, Weizmann Institute of Science ([email protected]) is Assistant Editor. The MPB is produced by Dr. Robert A. Werner, 3937 Blanche St., Pasadena, CA 91107 USA ([email protected]) and distributed by Derald D. Nye. Direct all subscriptions, contributions, address changes, etc. to:

Mr. Derald D. Nye - Minor Planet Bulletin 10385 East Observatory Drive Corona de Tucson, AZ 85641-2309 USA ([email protected]) (Telephone: 520-762-5504)

Effective with Volume 38, the Minor Planet Bulletin is a limited print journal, where print subscriptions are available only to libraries and major institutions for long-term archival purposes. In addition to the free electronic download of the MPB noted above, electronic retrieval of all Minor Planet Bulletin articles (back to Volume 1, Issue Number 1) is available through the Astrophysical Data System http://www.adsabs.harvard.edu/.

Authors should submit their manuscripts by electronic mail ([email protected]). Author instructions and a Microsoft Word template document are available at the web page given above. All materials must arrive by the deadline for each issue. Visual photometry observations, positional observations, any type of observation not covered above, and general information requests should be sent to the Coordinator.

* * * * *

The deadline for the next issue (45-1) is October 15, 2017. The deadline for issue 45-2 is January 15, 2018.

Minor Planet Bulletin 44 (2017)